Author name code: shine ADS astronomy entries on 2022-09-14 author:"Shine, Richard A." ------------------------------------------------------------------------ Title: The Hinode Spectro-Polarimeter Authors: Lites, B. W.; Akin, D. L.; Card, G.; Cruz, T.; Duncan, D. W.; Edwards, C. G.; Elmore, D. F.; Hoffmann, C.; Katsukawa, Y.; Katz, N.; Kubo, M.; Ichimoto, K.; Shimizu, T.; Shine, R. A.; Streander, K. V.; Suematsu, A.; Tarbell, T. D.; Title, A. M.; Tsuneta, S. Bibcode: 2013SoPh..283..579L Altcode: The joint Japan/US/UK Hinode mission includes the first large-aperture visible-light solar telescope flown in space. One component of the Focal Plane Package of that telescope is a precision spectro-polarimeter designed to measure full Stokes spectra with the intent of using those spectra to infer the magnetic-field vector at high precision in the solar photosphere. This article describes the characteristics of the flight hardware of the HinodeSpectro-Polarimeter, and summarizes its in-flight performance. Title: Interaction of Cometary Material With the Solar Corona: EUV Observations and MHD Simulations Authors: Liu, W.; Jia, Y.; Downs, C.; Schrijver, C.; Saint-Hilaire, P.; Battams, K.; Tarbell, T. D.; Shine, R. A. Bibcode: 2012AGUFMSH13B2254L Altcode: Extreme ultraviolet (EUV) emission from two recent sun-grazing comets, C/2011 N3 and C/2011 W3 (Lovejoy), has been observed in the solar corona for the first time by the SDO/AIA and STEREO/EUVI instruments (Schrijver et al. 2011). These observations provided a unique opportunity to investigate the interaction of the cometary material with the solar corona and probe their physical conditions. We present here EUV observations and MHD simulations on this subject, focusing on the deceleration of the cometary tail material within the corona. We found that despite their different local coronal environments, the two comets exhibited quite similar characteristics. The initial EUV emitting tail had a projected velocity of 100-200 km/s, which was much lower than the orbital velocity of 500-600 km/s in the plane-of-sky. This indicates that significant deceleration had taken place while the tail material was heated to coronal temperatures on the order of 1 MK before it started to emit in EUV (Bryans & Pesnell 2012). After its initial appearance, the tail further experienced a projected deceleration of ~1 km/s^2 (or 4 g_Sun). In particular, in the Lovejoy case, the tail appeared as clusters of bright parallel striations roughly at right angles to the orbit direction, suggestive of magnetic field lines illuminated by the plasma frozen onto them. These striations came to a stop and then accelerated in an opposite direction (seen in projection), approaching a constant velocity of ~50 km/s. These observations suggest that a Lorentz force from the coronal magnetic field was operating on the newly ionized cometary plasma. To test this hypothesis and understand tail deceleration mechanisms, we adopted a multi-fluid MHD model (Jia et al. 2012) to simulate the interaction between charged particles and the magnetized coronal plasma. We used potential extrapolation (Schrijver & DeRosa 2003) and a more sophisticated global MHD model (Lionello et al. 2009) to infer the magnetic field and plasma conditions of the corona along the comet's orbit as inputs to the simulations. We will compare the observations and simulation results, and discuss the implications for using sun-grazing comets as probes to the solar corona in the context of NASA's future Solar Probe Plus mission. Title: Signatures of Moving Magnetic Features in and above the Photosphere Authors: Hagenaar, H.; Shine, R.; Ryutova, M.; Dalda, A. S. Bibcode: 2012ASPC..454..181H Altcode: Hinode/SOT observations of NOAA AR 10933 from 2007 Jan 4 16:14 UT - Jan 6 22:20 UT are used to study MMFs (moving magnetic features) in the periphery of the region's large sunspot and the surrounding moat. The data consist of a nearly continuous set of Fe 6302 Å Stokes V images with sets of G band and Ca II H filtergrams at various cadences, FOV's, and resolutions plus some SpectroPolarimeter (SP) scans. We also used TRACE images in 171 Å to follow any possible signatures at higher temperatures. We applied automatic object recognition and tracking to the MMFs as seen in the Fe 6302 Å Stokes V images. An SP scan was used to determine the line profiles for several paths. Reliable inversions have not yet been done, but we find a few locations of possible supersonic downflows from the Stokes IQUV line profiles. The population of MMFs on the East side of the sunspot is much higher than on the opposite side, mostly involving a large number of mixed polarity MMFs. Consequently, the chromosphere shows strongly enhanced brightenings with a clear pattern: enhanced brightenings in Ca H outline the locations where opposite polarity MMFs meet. This activity does not prevent formation of active low lying “closed” loops at coronal temperatures seen in the TRACE 171 Å line. The other side, with fewer MMFs, shows a pattern that we found earlier: regions with an MMF deficiency show long living “open” coronal loops. This work was supported by NASA contract NNM07AA01C. Title: Some Like it Hot: the Trajectory of Sungrazing Comet C/2011 W3 (Lovejoy) in the Solar Neighborhood. Authors: Saint-Hilaire, Pascal; Chodas, P. W.; Battams, K.; Tarbell, T. D.; Shine, R. A.; Liu, W.; Thompson, W. T.; Comet Lovejoy Collaboration Team Bibcode: 2012AAS...22052107S Altcode: Sungrazing comet Lovejoy (C/2011 W3) was a recent spectacle in the sky, observed from the ground and by a host of space-based instruments, including several solar observatories. It is the first sungrazing comet in recent memory to have survived perihelion (q 1.2 Rs). It is only the second sungrazer to have been observed in the Sun's low corona in the extreme ultra-violet (EUV), where a plethora of EUV observations were obtained by the SDO and STEREO spacecraft. Such an occurrence can be used to probe the solar corona and test our understanding of plasma and cometary physics. In this work, we use the best orbit elements currently available to plot the path of the comet's nucleus on solar EUV images from SDO/AIA, both STEREO/EUVIs, and yellow continuum (near the Na D lines) images from Hinode/SOT. We compare the predicted positions and timing of the comet's nucleus to the latter, while the SDO and STEREO EUV observations are used to estimate the distance at which the EUV tail appears behind the comet's nucleus. Title: Wavelength Dependence of the Helioseismic and Magnetic Imager (HMI) Instrument onboard the Solar Dynamics Observatory (SDO) Authors: Couvidat, Sébastien; Schou, Jesper; Shine, Richard A.; Bush, Rock I.; Miles, John W.; Scherrer, Philip H.; Rairden, Richard L. Bibcode: 2012SoPh..275..285C Altcode: 2011SoPh..tmp..150C; 2011SoPh..tmp..219C; 2011SoPh..tmp...33C; 2011SoPh..tmp..110C The Helioseismic and Magnetic Imager (HMI) instrument will produce Doppler-velocity and vector-magnetic-field maps of the solar surface, whose accuracy is dependent on a thorough knowledge of the transmission profiles of the components of the HMI optical-filter system. Here we present a series of wavelength-dependence calibration tests, performed on the instrument from 2005 onwards, to obtain these profiles. We obtained the transmittances as a function of wavelength for the tunable and non-tunable filter elements, as well as the variation of these transmittances with temperature and the angle of incidence of rays of light. We also established the presence of fringe patterns produced by interferences inside the blocking filter and the front window, as well as a change in transmitted intensity with the tuning position. This thorough characterization of the HMI-filter system confirmed the very high quality of the instrument, and showed that its properties are well within the required specifications to produce superior data with high spatial and temporal resolution. Title: Initial Calibration of the Atmospheric Imaging Assembly (AIA) on the Solar Dynamics Observatory (SDO) Authors: Boerner, Paul; Edwards, Christopher; Lemen, James; Rausch, Adam; Schrijver, Carolus; Shine, Richard; Shing, Lawrence; Stern, Robert; Tarbell, Theodore; Title, Alan; Wolfson, C. Jacob; Soufli, Regina; Spiller, Eberhard; Gullikson, Eric; McKenzie, David; Windt, David; Golub, Leon; Podgorski, William; Testa, Paola; Weber, Mark Bibcode: 2012SoPh..275...41B Altcode: The Atmospheric Imaging Assembly (AIA) instrument onboard the Solar Dynamics Observatory (SDO) is an array of four normal-incidence reflecting telescopes that image the Sun in ten EUV and UV wavelength channels. We present the initial photometric calibration of AIA, based on preflight measurements of the response of the telescope components. The estimated accuracy is of order 25%, which is consistent with the results of comparisons with full-disk irradiance measurements and spectral models. We also describe the characterization of the instrument performance, including image resolution, alignment, camera-system gain, flat-fielding, and data compression. Title: Design and Ground Calibration of the Helioseismic and Magnetic Imager (HMI) Instrument on the Solar Dynamics Observatory (SDO) Authors: Schou, J.; Scherrer, P. H.; Bush, R. I.; Wachter, R.; Couvidat, S.; Rabello-Soares, M. C.; Bogart, R. S.; Hoeksema, J. T.; Liu, Y.; Duvall, T. L.; Akin, D. J.; Allard, B. A.; Miles, J. W.; Rairden, R.; Shine, R. A.; Tarbell, T. D.; Title, A. M.; Wolfson, C. J.; Elmore, D. F.; Norton, A. A.; Tomczyk, S. Bibcode: 2012SoPh..275..229S Altcode: The Helioseismic and Magnetic Imager (HMI) investigation (Solar Phys. doi:10.1007/s11207-011-9834-2, 2011) will study the solar interior using helioseismic techniques as well as the magnetic field near the solar surface. The HMI instrument is part of the Solar Dynamics Observatory (SDO) that was launched on 11 February 2010. The instrument is designed to measure the Doppler shift, intensity, and vector magnetic field at the solar photosphere using the 6173 Å Fe I absorption line. The instrument consists of a front-window filter, a telescope, a set of waveplates for polarimetry, an image-stabilization system, a blocking filter, a five-stage Lyot filter with one tunable element, two wide-field tunable Michelson interferometers, a pair of 40962 pixel cameras with independent shutters, and associated electronics. Each camera takes a full-disk image roughly every 3.75 seconds giving an overall cadence of 45 seconds for the Doppler, intensity, and line-of-sight magnetic-field measurements and a slower cadence for the full vector magnetic field. This article describes the design of the HMI instrument and provides an overview of the pre-launch calibration efforts. Overviews of the investigation, details of the calibrations, data handling, and the science analysis are provided in accompanying articles. Title: Monitoring Image Alignments and Flat Fields for AIA/SDO Data Images Authors: Shine, Richard A.; Wolfson, C.; Boerner, P. F.; Tarbell, T. D.; Nightingale, R. W. Bibcode: 2011SPD....42.2126S Altcode: 2011BAAS..43S.2126S The images from the 4 telescopes on the Atmospheric Imaging Assembly (AIA) on board the NASA Solar Dynamics Observatory (SDO) have different offsets (from sun center), plate scales, and absolute rotations that can be measured and corrected for accurate alignment. The most variable of these is the offsets presumably due to small thermal flexings of the telescopes. Here we describe the techniques used to make these measurements and show how the image alignments vary with time. Weekly measurements are made as part of the data monitoring that capture much of the drift in the geometric corrections but shorter time variations of typically a pixel also exist in the offsets. Angles and scales have much better short term stability. We hope to eventually capture these variations for the mission or at least provide software for end users.

We also describe progress made in determining flat fields for the 10 wavebands and show how these have been varying over the mission to date.

This work was supported by NASA under the SDO/AIA contract NNG04EA00C. Title: Temporal Relation Between the Disappearance of Penumbral Fine-scale Structure and Evershed Flow Authors: Kubo, M.; Ichimoto, K.; Lites, B. W.; Shine, R. A. Bibcode: 2011ApJ...731...84K Altcode: 2011arXiv1102.1137K We investigate the temporal relation between the Evershed flow, dot-like bright features (penumbral grain), the complex magnetic field structure, and dark lanes (dark core) along bright filaments in a sunspot penumbra. We use a time series of high spatial resolution photospheric intensity, vector magnetic field maps, and Doppler velocity maps obtained with the Solar Optical Telescope aboard the Hinode spacecraft. We conclude that the appearance and disappearance of the Evershed flow and penumbra grains occur at nearly the same time and are associated with changes of the inclination angle of the magnetic field from vertical to more horizontal. This supports the idea that Evershed flow is a result of thermal convection in the inclined field lines. The dark core of the bright penumbral filament also appears coincidental with the Evershed flow. However, the dark-cored bright filament survives at least for 10-20 minutes after the disappearance of the Evershed flow. The heat input into the bright filament continues even after the end of heat transfer by the Evershed flow. This suggests that local heating along the bright filament is important for maintaining its brightness, in addition to heat transfer by the Evershed flow. Title: Flat Fielding and Image Alignments for AIA/SDO Data Images Authors: Shine, R. A.; Nightingale, R. W.; Boerner, P.; Tarbell, T. D.; Wolfson, C. J. Bibcode: 2010AGUFMSH23C1872S Altcode: The Atmospheric Imaging Assembly (AIA) on the NASA Solar Dynamics Observatory (SDO) takes 4096 by 4096 CCD images of the sun in 10 wavelengths utilizing 4 telescopes and each wavelength channel requires a flat field that is applied shortly after receipt of the data on the ground. Although some useful information about the CCD's was obtained pre-launch, most of the flat field computation must be done with solar images taken in orbit. Raw flat field images are collected as out of focus images at 14 offsets using PZT adjustments on each telescope and then each wavelength group is processed together using the Kuhn, Lin, and Loranz (1991) flat field algorithm. However, the PZT motions are restricted to about 14 arc sec limiting the measurement of large scale variations. Hence larger offsets are also used by adjusting the space craft pointing. All of these suffer from changes in the solar image between exposures (especially the larger offsets), low counts in some channels, and reflections in the UV channels. These make direct use of the flats unfeasible and instead we process them to compute 6 separable effects: 1) differences in the CCD quad gains and inner row/column effects, 2) a repeating pattern across the CCD from the manufacturing process (dubbed "tire tracks"), 3) a grid pattern in the extreme ultraviolet wavelengths from the back filter, 4) blemishes (some are translucent and some are treated as bad pixels), 5) large scale vignetting, and 6) all other variations. The last category includes all remaining flat field effects after the others are removed. This has not been done well for any of the wavelengths yet. These effects will be described and illustrated, as will the before and after images resulting from applying the processed flat fields. We also describe techniques for fitting the solar limb to accurately determine image centers and radii. This is not a trivial problem for the extreme ultraviolet images but is required to align images, determine relative plate scales, and monitor pointing variations related to thermal changes. All channels except the He II 304A can be now be routinely measured with an rms error of typically less than 0.2 arc sec. This allows us to easily see the radius variations during the 24 hour orbit for example. The computer code requires about 3 seconds (single threaded) for each measurement. This work was supported by NASA under the SDO/AIA contract NNG04EA00C. Title: Coordinated observations of solar prominences with Hinode/SOT and SDO/AIA Authors: Berger, T. E.; Tarbell, T. D.; Schrijver, C. J.; Title, A. M.; Boerner, P.; Shine, R. A. Bibcode: 2010AGUFMSH21C..04B Altcode: We show the first detailed study of a solar quiescent prominence using simultaneous observations from the Hinode/SOT and SDO/AIA instruments. The prominence studied is a polar crown prominence located at the base of a large coronal cavity on the NW solar limb on 22-June-2010. Hinode observed the prominence for 2.75 hours running the HOP 73 prominence observation program to acquire Ca II H-line filtergrams and H-alpha doppler observations at a 20-second cadence. SOT observations in Ca II H-line and H-alpha spectral lines reveal the common dynamics of filamentary downflows and large-scale oscillations of the prominence body. In addition a dark cavity is observed to rise into the prominence and stagnate before going unstable to form Rayleigh-Taylor plume upflows. AIA observations in the 304, 171, 193, and 211 channels with 14 second cadence reveal that both the cavity and the plume upflows are bright in these hotter passbands. Filter ratio measurements as well as preliminary EM estimates imply that the cavity and plume plasma temperature is at least 10^6 K. Plasma at this temperature has never been detected or theorized in a confined configuration in the lower chromosphere below a prominence. Assuming an electron number density of 3e09 cm-3, the balance between thermal pressure in the cavity and magnetic pressure in the overlying prominence implies a magnetic flux density of order 10 gauss, in line with earlier measurements of prominence magnetic fields. However the cavity likely contains a significant magnetic energy density of its own implying that the prominence magnetic fields may need to be significantly higher to balance the cavity buoyancy. The existence of 10^6 K plasma confined below a quiescent prominence and the subsequent onset of buoyancy instabilities present new challenges to theories of prominence and coronal cavity formation and suggest new avenues for supply of mass and magnetic flux to the associated coronal cavity systems that make up the bulk of CMEs. Hinode/SOT Ca II H-line image overlain on SDO/AIA 304A image of a quiescent solar prominence. Title: Emergence of Helical Flux and the Formation of an Active Region Filament Channel Authors: Lites, B. W.; Kubo, M.; Berger, T.; Frank, Z.; Shine, R.; Tarbell, T.; Title, A.; Okamoto, T. J.; Otsuji, K. Bibcode: 2010ApJ...718..474L Altcode: We present comprehensive observations of the formation and evolution of a filament channel within NOAA Active Region (AR) 10978 from Hinode/Solar Optical Telescope and TRACE. We employ sequences of Hinode spectro-polarimeter maps of the AR, accompanying Hinode Narrowband Filter Instrument magnetograms in the Na I D1 line, Hinode Broadband Filter Instrument filtergrams in the Ca II H line and G-band, Hinode X-ray telescope X-ray images, and TRACE Fe IX 171 Å image sequences. The development of the channel resembles qualitatively that presented by Okamoto et al. in that many indicators point to the emergence of a pre-existing sub-surface magnetic flux rope. The consolidation of the filament channel into a coherent structure takes place rapidly during the course of a few hours, and the filament form then gradually shrinks in width over the following two days. Particular to this filament channel is the observation of a segment along its length of horizontal, weak (500 G) flux that, unlike the rest of the filament channel, is not immediately flanked by strong vertical plage fields of opposite polarity on each side of the filament. Because this isolated horizontal field is observed in photospheric lines, we infer that it is unlikely that the channel formed as a result of reconnection in the corona, but the low values of inferred magnetic fill fraction along the entire length of the filament channel suggest that the bulk of the field resides somewhat above the low photosphere. Correlation tracking of granulation in the G band presents no evidence for either systematic flows toward the channel or systematic shear flows along it. The absence of these flows, along with other indications of these data from multiple sources, reinforces (but does not conclusively demonstrate) the picture of an emerging flux rope as the origin of this AR filament channel. Title: Quiescent Prominence Dynamics Observed with the Hinode Solar Optical Telescope. I. Turbulent Upflow Plumes Authors: Berger, Thomas E.; Slater, Gregory; Hurlburt, Neal; Shine, Richard; Tarbell, Theodore; Title, Alan; Lites, Bruce W.; Okamoto, Takenori J.; Ichimoto, Kiyoshi; Katsukawa, Yukio; Magara, Tetsuya; Suematsu, Yoshinori; Shimizu, Toshifumi Bibcode: 2010ApJ...716.1288B Altcode: Hinode/Solar Optical Telescope (SOT) observations reveal two new dynamic modes in quiescent solar prominences: large-scale (20-50 Mm) "arches" or "bubbles" that "inflate" from below into prominences, and smaller-scale (2-6 Mm) dark turbulent upflows. These novel dynamics are related in that they are always dark in visible-light spectral bands, they rise through the bright prominence emission with approximately constant speeds, and the small-scale upflows are sometimes observed to emanate from the top of the larger bubbles. Here we present detailed kinematic measurements of the small-scale turbulent upflows seen in several prominences in the SOT database. The dark upflows typically initiate vertically from 5 to 10 Mm wide dark cavities between the bottom of the prominence and the top of the chromospheric spicule layer. Small perturbations on the order of 1 Mm or less in size grow on the upper boundaries of cavities to generate plumes up to 4-6 Mm across at their largest widths. All plumes develop highly turbulent profiles, including occasional Kelvin-Helmholtz vortex "roll-up" of the leading edge. The flows typically rise 10-15 Mm before decelerating to equilibrium. We measure the flowfield characteristics with a manual tracing method and with the Nonlinear Affine Velocity Estimator (NAVE) "optical flow" code to derive velocity, acceleration, lifetime, and height data for several representative plumes. Maximum initial speeds are in the range of 20-30 km s-1, which is supersonic for a ~10,000 K plasma. The plumes decelerate in the final few Mm of their trajectories resulting in mean ascent speeds of 13-17 km s-1. Typical lifetimes range from 300 to 1000 s (~5-15 minutes). The area growth rate of the plumes (observed as two-dimensional objects in the plane of the sky) is initially linear and ranges from 20,000 to 30,000 km2 s-1 reaching maximum projected areas from 2 to 15 Mm2. Maximum contrast of the dark flows relative to the bright prominence plasma in SOT images is negative and ranges from -10% for smaller flows to -50% for larger flows. Passive scalar "cork movies" derived from NAVE measurements show that prominence plasma is entrained by the upflows, helping to counter the ubiquitous downflow streams in the prominence. Plume formation shows no clear temporal periodicity. However, it is common to find "active cavities" beneath prominences that can spawn many upflows in succession before going dormant. The mean flow recurrence time in these active locations is roughly 300-500 s (5-8 minutes). Locations remain active on timescales of tens of minutes up to several hours. Using a column density ratio measurement and reasonable assumptions on plume and prominence geometries, we estimate that the mass density in the dark cavities is at most 20% of the visible prominence density, implying that a single large plume could supply up to 1% of the mass of a typical quiescent prominence. We hypothesize that the plumes are generated from a Rayleigh-Taylor instability taking place on the boundary between the buoyant cavities and the overlying prominence. Characteristics, such as plume size and frequency, may be modulated by the strength and direction of the cavity magnetic field relative to the prominence magnetic field. We conclude that buoyant plumes are a source of quiescent prominence mass as well as a mechanism by which prominence plasma is advected upward, countering constant gravitational drainage. Title: High Velocity Horizontal Motions at the Edge of Sunspot Penumbrae Authors: Hagenaar-Daggett, Hermance J.; Shine, R. Bibcode: 2010AAS...21640110H Altcode: 2010BAAS...41R.858H The outer edges of sunspot penumbrae have long been noted as a region of interesting dynamics including formation of MMFs, extensions and retractions of the penumbral tips, fast moving (2-3 km/s) bright features dubbed"streakers", and localized regions of high speed downflows interpreted as Evershed "sinks". Using 30s cadence movies of high spatial resolution G band and Ca II H images taken by the Hinode SOT/FPP instrument from 5-7 Jan 2007, we have been investigating the penumbra around a sunspot in AR 10933. In addition to the expected phenomena, we also see occasional small dark crescent-shaped features with high horizontal velocities (6.5 km/s) in G band movies. These appear to be emitted from penumbral tips. They travel about 1.5 Mm developing a bright wake that evolves into a slower moving (1-2 km/s) bright feature. In some cases, there may be an earlier outward propagating disturbance within the penumbra. We have also analyzed available Fe 6302 Stokes V images to obtain information on the magnetic field. Although only lower resolution 6302 images made with a slower cadence are available for these particular data sets, we can establish that the features have the opposite magnetic polarity of the sunspot. This observation may be in agreement with simulations showing that a horizontal flux tube develops crests that move outward with a velocity as large as 10 km/s.

This work was supported by NASA contract NNM07AA01C. Title: Is Flux Submergence an Essential Aspect of Flux Emergence? Authors: Lites, B. W.; Frank, Z.; Shine, R. A.; Title, A. M.; Ichimoto, K. Bibcode: 2009ASPC..415..172L Altcode: High resolution Hinode Spectro-Polarimeter observations permit one to examine the detailed structure of the magnetic field vector in emerging flux regions. We find the field to have a concave-upward geometry on the smallest scales observed (0.3 arcsec), indicating the presence of U-loops at the sites of approaching and canceling opposite polarities. This structure suggests that reconnection is taking place at or below the surface, allowing the emerging flux to rid itself of its considerable mass burden. Supersonic down flows are often observed adjacent to, but not coincident with, the sites of canceling flux. We propose that these are the sites that drain the mass contained in the buoyantly-rising flux elements. The observations then suggest a process of sub-surface reconnection producing O-loops that then are forced to descend with the intergranular convective down flows, thus making flux submergence important to the larger scale flux emergence process. Title: Moving Magnetic Features and the Flow Pattern around Sunspots Authors: Hagenaar, H. J.; Shine, R. A. Bibcode: 2009AGUFMSH51A1255H Altcode: Studies of Moving Magnetic Features indicate a Spoke Pattern around Sunspots. We investigate this flow pattern further on Hinode/ SOT data. Title: Helical Shape and Twisting Motion as Intrinsic Properties of Penumbral Filaments Authors: Shine, R. A.; Ryutova, M.; Berger, T. E.; Title, A. M.; Tarbell, T. D.; Ichimoto, K. Bibcode: 2009AGUFMSH23B1541S Altcode: A wealth of high resolution data obtained with advanced ground based telescopes and the SOT instrument on HINODE have led to new findings in the properties of penumbral filaments and controversies in their interpretation. Here we address one such issue, namely the question of whether the apparent twist of filaments is real or is just a viewing effect. We show that the helical shape and twisting motions of penumbral filaments follow from first principles and represent an integral part of penumbra formation and dynamics. As such, these properties link together other observed features of filaments including their magnetic and thermal substructure and their impact on the overlying atmosphere. At all stages of penumbral dynamics, qualitative agreement of theory and observations is supported by quantitative analysis as well. Title: A New View of Fine Scale Dynamics and Magnetism of Sunspots Revealed by Hinode/SOT Authors: Ichimoto, K.; Suematsu, Y.; Katsukawa, Y.; Tsuneta, S.; Shimojo, M.; Shimizu, T.; Shine, R. A.; Tarbell, T. D.; Berger, T.; Title, A. M.; Lites, B. W.; Kubo, M.; Yokoyama, T.; Nagata, S. Bibcode: 2009ASPC..405..167I Altcode: The Solar Optical Telescope on-board Hinode is providing a new view of the fine scale dynamics in sunspots with its high spatial resolution and unprecedented image stability. We present three features related to the Evershed flow each of which raises a new puzzle in sunspot dynamics; i.e., twisting appearance of penumbral filaments, the source and sink of individual Evershed flow channels, and the net circular polarization in penumbrae with its spatial relation to the Evershed flow channels. Title: Has Hinode Revealed the Missing Turbulent Flux of the Quiet Sun? Authors: Lites, B. W.; Kubo, M.; Socas-Navarro, H.; Berger, T.; Frank, Z.; Shine, R.; Tarbell, T.; Title, A. M.; Ichimoto, K.; Katsukawa, Y.; Tsuneta, S.; Suematsu, Y.; Shimizu, T.; Nagata, S. Bibcode: 2009ASPC..405..173L Altcode: The Hinode Spectro-Polarimeter has revealed the presence of surprisingly strong horizontal magnetic fields nearly everywhere in the quiet solar atmosphere. These horizontal fields, along with measures of the vertical fields, may be the signature of the ``hidden turbulent flux'' of the quiet Sun. The measured horizontal fields average at least to 55 Gauss: nearly 5 times that of the measured longitudinal apparent flux density. The nature of these fields are reviewed, and discussed in the light of recent magneto-convection numerical simulations of the quiet Sun. Title: Hinode Observation of the Magnetic Fields in a Sunspot Light Bridge Accompanied by Long-Lasting Chromospheric Plasma Ejections Authors: Shimizu, Toshifumi; Katsukawa, Yukio; Kubo, Masahito; Lites, Bruce W.; Ichimoto, Kiyoshi; Suematsu, Yoshinori; Tsuneta, Saku; Nagata, Shin'ichi; Shine, Richard A.; Tarbell, Theodore D. Bibcode: 2009ApJ...696L..66S Altcode: We present high-resolution magnetic field measurements of a sunspot light bridge (LB) that produced chromospheric plasma ejections intermittently and recurrently for more than 1 day. The observations were carried out with the Hinode Solar Optical Telescope on 2007 April 29 and 30. The spectro-polarimeter reveals obliquely oriented magnetic fields with vertical electric current density higher than 100 mA m-2 along the LB. The observations suggest that current-carrying highly twisted magnetic flux tubes are trapped below a cusp-shaped magnetic structure along the LB. The presence of trapped current-carrying flux tubes is essential for causing long-lasting chromospheric plasma ejections at the interface with pre-existing vertically oriented umbral fields. A bidirectional jet was clearly detected, suggesting magnetic reconnections occurring at very low altitudes, slightly above the height where the vector magnetic fields are measured. Moreover, we found another strong vertical electric current on the interface between the current-carrying flux tube and pre-existing umbral field, which might be a direct detection of the currents flowing in the current sheet formed at the magnetic reconnection sites. Title: Magnetic Feature Tracking in Sunspot Moats Using Hinode/SOT Observations Authors: Hagenaar-Daggett, Hermance J.; Shine, R. A.; Tarbell, T. D. Bibcode: 2009SPD....40.0908H Altcode: A long series of continuous observations of NOAA AR 10933 taken by Hinode/SOT from 2-4 January, 2007 is used to study MMF's (moving magnetic features) in the periphery of the large sunspot in the region and its surrounding moat. We describe some algorithms we have developed to quickly recognize and track discrete features and apply these to the magnetic structures seen in Na I 589.6nm Stokes V images. Because the features evolve and show variable visibilty, automatic tracking is not always successful even with the seeing free Hinode images and we are still attempting to improve our techniques. We also compute flow maps from the photospheric G band images using LCT (local correlation tracking) to compare with the generally faster MMF motions.

This work was supported by NASA contract NNM07AA01C. Title: Prominence Formation Associated with an Emerging Helical Flux Rope Authors: Okamoto, Takenori J.; Tsuneta, Saku; Lites, Bruce W.; Kubo, Masahito; Yokoyama, Takaaki; Berger, Thomas E.; Ichimoto, Kiyoshi; Katsukawa, Yukio; Nagata, Shin'ichi; Shibata, Kazunari; Shimizu, Toshifumi; Shine, Richard A.; Suematsu, Yoshinori; Tarbell, Theodore D.; Title, Alan M. Bibcode: 2009ApJ...697..913O Altcode: 2009arXiv0904.0007O The formation and evolution process and magnetic configuration of solar prominences remain unclear. In order to study the formation process of prominences, we examine continuous observations of a prominence in NOAA AR 10953 with the Solar Optical Telescope on the Hinode satellite. As reported in our previous Letter, we find a signature suggesting that a helical flux rope emerges from below the photosphere under a pre-existing prominence. Here we investigate more detailed properties and photospheric indications of the emerging helical flux rope, and discuss their relationship to the formation of the prominence. Our main conclusions are: (1) a dark region with absence of strong vertical magnetic fields broadens and then narrows in Ca II H-line filtergrams. This phenomenon is consistent with the emergence of the helical flux rope as photospheric counterparts. The size of the flux rope is roughly 30,000 km long and 10,000 km wide. The width is larger than that of the prominence. (2) No shear motion or converging flows are detected, but we find diverging flows such as mesogranules along the polarity inversion line. The presence of mesogranules may be related to the emergence of the helical flux rope. (3) The emerging helical flux rope reconnects with magnetic fields of the pre-existing prominence to stabilize the prominence for the next several days. We thus conjecture that prominence coronal magnetic fields emerge in the form of helical flux ropes that contribute to the formation and maintenance of the prominence. Title: The Magnetic Landscape of the Sun's Polar Region Authors: Tsuneta, S.; Ichimoto, K.; Katsukawa, Y.; Lites, B. W.; Matsuzaki, K.; Nagata, S.; Orozco Suárez, D.; Shimizu, T.; Shimojo, M.; Shine, R. A.; Suematsu, Y.; Suzuki, T. K.; Tarbell, T. D.; Title, A. M. Bibcode: 2008ApJ...688.1374T Altcode: 2008arXiv0807.4631T We present observations of the magnetic landscape of the polar region of the Sun that are unprecedented in terms of spatial resolution, field of view, and polarimetric precision. They were carried out with the Solar Optical Telescope aboard Hinode. Using a Milne-Eddington inversion, we find many vertically oriented magnetic flux tubes with field strengths as strong as 1 kG scattered in latitude between 70° and 90°. They all have the same polarity, consistent with the global polarity of the polar region. The field vectors are observed to diverge from the centers of the flux elements, consistent with a view of magnetic fields that are expanding and fanning out with height. The polar region is also found to have ubiquitous horizontal fields. The polar regions are the source of the fast solar wind, which is channeled along unipolar coronal magnetic fields whose photospheric source is evidently rooted in the strong-field, vertical patches of flux. We conjecture that vertical flux tubes with large expansion around the photospheric-coronal boundary serve as efficient chimneys for Alfvén waves that accelerate the solar wind. Title: Magnetic Fields of the Quiet Sun: A New Quantitative Perspective From Hinode Authors: Lites, B. W.; Kubo, M.; Socas-Navarro, H.; Berger, T.; Frank, Z.; Shine, R.; Tarbell, T.; Title, A.; Ichimoto, K.; Katsukawa, Y.; Tsuneta, S.; Suematsu, Y.; Shimizu, T.; Nagata, S. Bibcode: 2008ASPC..397...17L Altcode: This article summarizes results of studies presented in two papers already published: Lites et al. (2007a); Lites et al. (2007b). Please see these for further details. Title: On-orbit Performance of the Solar Optical Telescope aboard Hinode Authors: Ichimoto, K.; Katsukawa, Y.; Tarbell, T.; Shine, R. A.; Hoffmann, C.; Berger, T.; Cruz, T.; Suematsu, Y.; Tsuneta, S.; Shimizu, T.; Lites, B. W. Bibcode: 2008ASPC..397....5I Altcode: 2008arXiv0804.3248I On-orbit performance of the Solar Optical Telescope (SOT) aboard Hinode is described with some attention to its unpredicted aspects. In general, SOT reveals an excellent performance and has been providing outstanding data. Some unexpected features exist, however, in behaviours of the focus position, throughput and structural stability. Most of them are recovered by the daily operation i.e., frequent focus adjustment, careful heater setting and corrections in data analysis. The tunable filter contains air bubbles which degrade the data quality significantly. Schemes for tuning the filter without disturbing the bubbles have been developed and tested, and some useful procedures to obtain Dopplergrams and magnetograms are now available. October and March, when the orbit of satellite becomes nearly perpendicular to the direction towards the Sun, provide a favourable condition for continuous runs of the narrow-band filter imager. Title: High Resolution Observations of Spicules with Hinode/SOT Authors: Suematsu, Y.; Ichimoto, K.; Katsukawa, Y.; Shimizu, T.; Okamoto, T.; Tsuneta, S.; Tarbell, T.; Shine, R. A. Bibcode: 2008ASPC..397...27S Altcode: High time cadence unprecedented images at the limb with Ca II H line filtergraph from the Solar Optical Telescope (SOT) aboard Hinode have revealed that a spicule consists of highly dynamic multi-threads (typically twin) as thin as a few tenths of an arcsecond, and shows prominent lateral movement or oscillation with rotation on its axis during its life. This multi-thread structure and lateral motion indicate that the spicules can be driven by magnetic reconnection at unresolved spatial scales at their footpoints. Title: Evolution of Magnetic Fields at the Boundary of the Penumbra Authors: Kubo, M.; Ichimoto, K.; Shimizu, T.; Lites, B. W.; Tsuneta, S.; Suematsu, Y.; Katsukawa, Y.; Nagata, S.; Tarbell, T.; Shine, R. A.; Title, A. M. Bibcode: 2008ASPC..397...79K Altcode: The formation of moving magnetic features (MMFs) separating from the penumbra were successfully observed with the Solar Optical Telescope (SOT) aboard the Hinode satellite. We find that bright features in the outer penumbra are located at the penumbral spines, which have magnetic fields more vertical than the surroundings, or located at the MMFs separating from the spines. This suggests that convection in the outer penumbra is related to the disintegration of the sunspot. Title: Disintegration of Magnetic Flux in Decaying Sunspots as Observed with the Hinode SOT Authors: Kubo, M.; Lites, B. W.; Ichimoto, K.; Shimizu, T.; Suematsu, Y.; Katsukawa, Y.; Tarbell, T. D.; Shine, R. A.; Title, A. M.; Nagata, S.; Tsuneta, S. Bibcode: 2008ApJ...681.1677K Altcode: 2008arXiv0806.0415K Continuous observations of sunspot penumbrae with the Solar Optical Telescope aboard Hinode clearly show that the outer boundary of the penumbra fluctuates around its averaged position. The penumbral outer boundary moves inward when granules appear in the outer penumbra. We discover that such granules appear one after another while moving magnetic features (MMFs) are separating from the penumbral "spines" (penumbral features that have fields that are stronger and more vertical than those of their surroundings). These granules that appear in the outer penumbra often merge with bright features inside the penumbra that move with the spines as they elongate toward the moat region. This suggests that convective motions around the penumbral outer boundary are related to the disintegration of magnetic flux in the sunspot. We also find that dark penumbral filaments frequently elongate into the moat region in the vicinity of MMFs that detach from penumbral spines. Such elongating dark penumbral filaments correspond to nearly horizontal fields extending from the penumbra. Pairs of MMFs with positive and negative polarities are sometimes observed along the elongating dark penumbral filaments. This strongly supports the notion that such elongating dark penumbral filaments have magnetic fields with a "sea serpent"-like structure. Evershed flows, which are associated with the penumbral horizontal fields, may be related to the detachment of the MMFs from the penumbral spines, as well as to the formation of the MMFs along the dark penumbral filaments that elongate into the moat region. Title: Polarization Calibration of the Solar Optical Telescope onboard Hinode Authors: Ichimoto, K.; Lites, B.; Elmore, D.; Suematsu, Y.; Tsuneta, S.; Katsukawa, Y.; Shimizu, T.; Shine, R.; Tarbell, T.; Title, A.; Kiyohara, J.; Shinoda, K.; Card, G.; Lecinski, A.; Streander, K.; Nakagiri, M.; Miyashita, M.; Noguchi, M.; Hoffmann, C.; Cruz, T. Bibcode: 2008SoPh..249..233I Altcode: 2008SoPh..tmp...69I The Solar Optical Telescope (SOT) onboard Hinode aims to obtain vector magnetic fields on the Sun through precise spectropolarimetry of solar spectral lines with a spatial resolution of 0.2 - 0.3 arcsec. A photometric accuracy of 10−3 is achieved and, after the polarization calibration, any artificial polarization from crosstalk among Stokes parameters is required to be suppressed below the level of the statistical noise over the SOT's field of view. This goal was achieved by the highly optimized design of the SOT as a polarimeter, extensive analyses and testing of optical elements, and an end-to-end calibration test of the entire system. In this paper we review both the approach adopted to realize the high-precision polarimeter of the SOT and its final polarization characteristics. Title: Image Stabilization System for Hinode (Solar-B) Solar Optical Telescope Authors: Shimizu, T.; Nagata, S.; Tsuneta, S.; Tarbell, T.; Edwards, C.; Shine, R.; Hoffmann, C.; Thomas, E.; Sour, S.; Rehse, R.; Ito, O.; Kashiwagi, Y.; Tabata, M.; Kodeki, K.; Nagase, M.; Matsuzaki, K.; Kobayashi, K.; Ichimoto, K.; Suematsu, Y. Bibcode: 2008SoPh..249..221S Altcode: The Hinode Solar Optical Telescope (SOT) is the first space-borne visible-light telescope that enables us to observe magnetic-field dynamics in the solar lower atmosphere with 0.2 - 0.3 arcsec spatial resolution under extremely stable (seeing-free) conditions. To achieve precise measurements of the polarization with diffraction-limited images, stable pointing of the telescope (<0.09 arcsec, 3σ) is required for solar images exposed on the focal plane CCD detectors. SOT has an image stabilization system that uses image displacements calculated from correlation tracking of solar granules to control a piezo-driven tip-tilt mirror. The system minimizes the motions of images for frequencies lower than 14 Hz while the satellite and telescope structural design damps microvibration in higher frequency ranges. It has been confirmed from the data taken on orbit that the remaining jitter is less than 0.03 arcsec (3σ) on the Sun. This excellent performance makes a major contribution to successful precise polarimetric measurements with 0.2 - 0.3 arcsec resolution. Title: The Solar Optical Telescope for the Hinode Mission: An Overview Authors: Tsuneta, S.; Ichimoto, K.; Katsukawa, Y.; Nagata, S.; Otsubo, M.; Shimizu, T.; Suematsu, Y.; Nakagiri, M.; Noguchi, M.; Tarbell, T.; Title, A.; Shine, R.; Rosenberg, W.; Hoffmann, C.; Jurcevich, B.; Kushner, G.; Levay, M.; Lites, B.; Elmore, D.; Matsushita, T.; Kawaguchi, N.; Saito, H.; Mikami, I.; Hill, L. D.; Owens, J. K. Bibcode: 2008SoPh..249..167T Altcode: 2008SoPh..tmp...74T; 2007arXiv0711.1715T The Solar Optical Telescope (SOT) aboard the Hinode satellite (formerly called Solar-B) consists of the Optical Telescope Assembly (OTA) and the Focal Plane Package (FPP). The OTA is a 50-cm diffraction-limited Gregorian telescope, and the FPP includes the narrowband filtergraph (NFI) and the broadband filtergraph (BFI), plus the Stokes Spectro-Polarimeter (SP). The SOT provides unprecedented high-resolution photometric and vector magnetic images of the photosphere and chromosphere with a very stable point spread function and is equipped with an image-stabilization system with performance better than 0.01 arcsec rms. Together with the other two instruments on Hinode (the X-Ray Telescope (XRT) and the EUV Imaging Spectrometer (EIS)), the SOT is poised to address many fundamental questions about solar magnetohydrodynamics. This paper provides an overview; the details of the instrument are presented in a series of companion papers. Title: Frequent Occurrence of High-Speed Local Mass Downflows on the Solar Surface Authors: Shimizu, T.; Lites, B. W.; Katsukawa, Y.; Ichimoto, K.; Suematsu, Y.; Tsuneta, S.; Nagata, S.; Kubo, M.; Shine, R. A.; Tarbell, T. D. Bibcode: 2008ApJ...680.1467S Altcode: 2008arXiv0804.1167S We report on new spectropolarimetric measurements with simultaneous filter imaging observation, revealing the frequent appearance of polarization signals indicating high-speed, probably supersonic, downflows that are associated with at least three different configurations of magnetic fields in the solar photosphere. The observations were carried out with the Solar Optical Telescope on board the Hinode satellite. High-speed downflows are excited when a moving magnetic feature is newly formed near the penumbral boundary of sunspots. Also, a new type of downflows is identified at the edge of sunspot umbra that lack accompanying penumbral structures. These may be triggered by the interaction of magnetic fields swept by convection with well-concentrated magnetic flux. Another class of high-speed downflows are observed in quiet Sun and sunspot moat regions. These are closely related to the formation of small concentrated magnetic flux patches. High-speed downflows of all types are transient time-dependent mass motions. These findings suggest that the excitation of supersonic mass flows are one of the key observational features of the dynamical evolution occurring in magnetic-field fine structures on the solar surface. Title: Cooperative Observation of Ellerman Bombs between the Solar Optical Telescope aboard Hinode and Hida/Domeless Solar Telescope Authors: Matsumoto, Takuma; Kitai, Reizaburo; Shibata, Kazunari; Nagata, Shin'ichi; Otsuji, Kenichi; Nakamura, Tahei; Watanabe, Hiroko; Tsuneta, Saku; Suematsu, Yoshinori; Ichimoto, Kiyoshi; Shimizu, Toshifumi; Katsukawa, Yukio; Tarbell, Theodore D.; Lites, Bruce W.; Shine, Richard A.; Title, Alan M. Bibcode: 2008PASJ...60..577M Altcode: High-resolution CaIIH broad-band filter images of NOAA10933 on 2007 January 5 were obtained by the Solar Optical Telescope aboard the Hinode satellite. Many small-scale (∼1") bright points were observed outside the sunspot and inside the emerging flux region. We identified some of these bright points with Ellerman bombs (EBs) by using Hα images taken by the Domeless Solar Telescope at Hida observatory. The sub-arcsec structures of two EBs seen in CaIIH were studied in detail. Our observation showed the following two aspects: (1) The CaIIH bright points identified with EBs were associated with the bipolar magnetic field structures, as reported by previous studies. (2)The structure of the CaIIH bright points turned out to consist of the following two parts: a central elongated bright core (0.7" × 0.5") located along the magnetic neutral line and a diffuse halo (1.2"×1.8"). Title: Emergence of a helical flux rope and prominence formation Authors: Okamoto, T. J.; Tsuneta, S.; Lites, B. W.; Kubo, M.; Yokoyama, T.; Berger, T. E.; Ichimoto, K.; Katsukawa, Y.; Nagata, S.; Shibata, K.; Shimizu, T.; Shine, R. A.; Suematsu, Y.; Tarbell, T. D.; Title, A. M. Bibcode: 2008AGUSMSP43B..06O Altcode: We report a discovery about emergence of a helical flux rope. The episode may be related to the formation and evolution of an active region prominence. Statistical studies by previous authors indicate that numerous prominences have the inverse-polarity configuration suggesting the helical magnetic configurations. There are two theoretical models about formation of such a coronal helical magnetic field in association with prominences: flux rope model and sheared-arcade model. We have so far no clear observational evidence to support either model. In order to find a clue about the formation of the prominence, we had continuous observations of NOAA AR 10953 with the SOT during 2007 April 28 to May 9. A prominence was located over the polarity inversion line in the south-east of the main sunspot. These observations provided us with a time series of vector magnetic fields on the photosphere under the prominence. We found four new features: (1) The abutting opposite-polarity regions on the two sides along the polarity inversion line first grew laterally in size and then narrowed. (2) These abutting regions contained vertically-weak, but horizontally-strong magnetic fields. (3) The orientations of the horizontal magnetic fields along the polarity inversion line on the photosphere gradually changed with time from a normal- polarity configuration to an inverse-polarity one. (4) The horizontal-magnetic field region was blueshifted. These indicate that helical flux rope emerges from below the photosphere into the corona along the polarity inversion line under the prominence. We suggest that this supply of a helical magnetic flux possibly into the corona is related to formation and maintenance of active-region prominences. Title: Photospheric Signature of Penumbral Microjets Authors: Katsukawa, Y.; Jurcak, J.; Ichimoto, K.; Suemtasu, Y.; Tsuneta, S.; Shimizu, T.; Berger, T. E.; Shine, R. A.; Tarbell, T. D.; Lites, B. W. Bibcode: 2008AGUSMSP53A..03K Altcode: HINODE Solar Optical Telescope (SOT) discovered ubiquitous occurrence of fine-scale jetlike activities in penumbral chromospheres, which are referred to as penumbral microjets. The microjets' small width of 400 km and short duration of less than 1 min make them difficult to identify in existing ground-based observations. The apparent rise velocity is faster than 50km/s and is roughly comparable to the Alfven speed in the sunspot chromosphere. These properties of penumbral microjets suggest that magnetic reconnection in uncombed magnetic field configuration is the most possible cause of penumbral microjets. In order to understand magnetic configuration associated with penumbral microjets and prove the chromospheric magnetic reconnection hypothesis, we investigated relationship between penumbral microjets seen in CaIIH images and photospheric magnetic fields measured by the HINODE spectro-polarimeter. We found the inclination angles of penumbral microjets measured in CaII H images are roughly consistent with inclination angles of relatively vertical magnetic field component in uncombed magnetic field configuration. In addition, strong and transient downflows are observed in the photosphere near the boundary of a horizontal flux tube associated with a penumbral microjet. The size of the downflow region is about 300km, which is close to the width of penumbral microjets seen in CaII H images. The downflow velocity of several km/s might be a result of an outflow of chromospheric magnetic reconnection and suffer deceleration due to the higher density in the photosphere. Title: Evolution of Evershed and Shear Flows Associated With the X3.4 Flare of December 13, 2006 Authors: Tan, C.; Shine, R. A.; Abramenko, V. I.; Wang, H. Bibcode: 2008AGUSMSP51C..03T Altcode: Liu et al. (2006) presented the observation of rapid penumbra decay associated with a number of X-class flares. As the Evershed flows are closely associated with morphology of sunspot penumbra, in this work, we use the state-of-art Hinode data to track Evershed flow in flaring active regions as well as shear flows close to the flaring neutral line. This paper concentrates on the study of AR10930 around the time of the X3.4 flare time on December 13, 2006. We utilize the seeing-free data from Hinode SOT G-band data as the tracer to obtain the horizontal component of the Evershed flows by local correlation tracking. We find that: (1) The penumbra decay appears obviously in this active region associated with the X3.4 flare. (2) The Evershed flow decreases slightly immediately following the flare, indicating that magnetic fields become more vertical associated with the flare. In addition, we will discuss the evolution of shear flows near the neutral line of this delta spot leading to and following the flare. Title: Sources and Sinks of the Evershed Flow Authors: Shine, R. A.; Title, A. M.; Ichimoto, K.; Lites, B. Bibcode: 2008AGUSMSP31A..01S Altcode: Extending the work of Ichimoto et al (2007), we investigate the sources and sinks of the Evershed flow in sunspot penumbra using data from the Solar Optical Telescope (SOT) instruments on the Hinode satellite. We use spectral maps taken with the Spectro-Polarimeter (SP) that provide detailed snapshots of the large sunspot in AR 10930 over a range of viewing angles as it rotated across the solar disk in December 2006. These are supplemented by images taken with the Filtergraph (FG) instrument that show the dynamics of the structures. AR 10930 has some large sunspots showing sources and sinks within the penumbra as well as near the inner and outer boundaries. There are also regions of contact between penumbra of two sunspots (of opposite magnetic polarity) that show stronger horizontal flows and downdrafts than seen elsewhere in the penumbras. The relationship between Evershed "clouds" showing quasi-periodic variations in the spatially averaged Evershed flow and the penumbral fine structures is also investigated. This work was supported by NASA contract NNM07AA01C. Title: Disintegration of Magnetic Flux in Decaying Sunspots as Observed with the Hinode/SOT Authors: Kubo, M.; Lites, B. W.; Ichimoto, K.; Shimizu, T.; Suematsu, Y.; Katsukawa, Y.; Tarbell, T. D.; Shine, R. A.; Title, A. M.; Nagata, S.; Tsuneta, S. Bibcode: 2008AGUSMSP31B..01K Altcode: Continuous observations of sunspot penumbrae with the Solar Optical Telescope aboard Hinode clearly show that the outer boundary of the penumbra fluctuates around its averaged position. The penumbral outer boundary moves inward when granules appear in the outer penumbra. We discover that such granules appear one after another while moving magnetic features (MMFs) are separating from the penumbral "spines" (penumbral features having fields that are stronger and more vertical than their surroundings). These granules that appear in the outer penumbra often merge with bright features inside the penumbra that move with spines as they elongate toward the moat region. This suggests that convective motions around the penumbral outer boundary are related to disintegration of magnetic flux in the sunspot. We also find that dark penumbral filaments frequently elongate into the moat region in the vicinity of MMFs that detach from penumbral spines. Such elongating dark penumbral filaments correspond to nearly horizontal fields extending from the penumbra. Pairs of MMFs with positive and negative polarities are sometimes observed along the elongating dark penumbral filaments. This strongly supports the notion that such elongating dark penumbral filaments have magnetic fields with a "sea serpent"-like structure. Evershed flows, which are associated with the penumbral horizontal fields, may be related to detachment of the MMFs from the penumbral spines, as well as to the formation of the MMFs along the dark penumbral filaments that elongate into the moat region. Title: Formation of Solar Magnetic Flux Tubes with Kilogauss Field Strength Induced by Convective Instability Authors: Nagata, Shin'ichi; Tsuneta, Saku; Suematsu, Yoshinori; Ichimoto, Kiyoshi; Katsukawa, Yukio; Shimizu, Toshifumi; Yokoyama, Takaaki; Tarbell, Theodore D.; Lites, Bruce W.; Shine, Richard A.; Berger, Thomas E.; Title, Alan M.; Bellot Rubio, Luis R.; Orozco Suárez, David Bibcode: 2008ApJ...677L.145N Altcode: Convective instability has been a mechanism used to explain the formation of solar photospheric flux tubes with kG field strength. However, the turbulence of the Earth's atmosphere has prevented ground-based observers from examining the hypothesis with precise polarimetric measurement on the subarcsecond scale flux tubes. Here we discuss observational evidence of this scenario based on observations with the Solar Optical Telescope (SOT) aboard Hinode. The cooling of an equipartition field strength flux tube precedes a transient downflow reaching 6 km s-1 and the intensification of the field strength to 2 kG. These observations agree very well with the theoretical predictions. Title: Transient horizontal magnetic fields in solar plage regions Authors: Ishikawa, R.; Tsuneta, S.; Ichimoto, K.; Isobe, H.; Katsukawa, Y.; Lites, B. W.; Nagata, S.; Shimizu, T.; Shine, R. A.; Suematsu, Y.; Tarbell, T. D.; Title, A. M. Bibcode: 2008A&A...481L..25I Altcode: 2008arXiv0802.1769I Aims:We report the discovery of isolated, small-scale emerging magnetic fields in a plage region with the Solar Optical Telescope aboard Hinode.
Methods: Spectro-polarimetric observations were carried out with a cadence of 34 s for the plage region located near disc center. The vector magnetic fields are inferred by Milne-Eddington inversion.
Results: The observations reveal widespread occurrence of transient, spatially isolated horizontal magnetic fields. The lateral extent of the horizontal magnetic fields is comparable to the size of photospheric granules. These horizontal magnetic fields seem to be tossed about by upflows and downflows of the granular convection. We also report an event that appears to be driven by the magnetic buoyancy instability. We refer to buoyancy-driven emergence as type 1 and convection-driven emergence as type 2. Although both events have magnetic field strengths of about 600 G, the filling factor of type 1 is a factor of two larger than that of type 2.
Conclusions: Our finding suggests that the granular convection in the plage regions is characterized by a high rate of occurrence of granular-sized transient horizontal fields. Title: Net circular polarization of sunspots in high spatial resolution Authors: Ichimoto, K.; Tsuneta, S.; Suematsu, Y.; Katsukawa, Y.; Shimizu, T.; Lites, B. W.; Kubo, M.; Tarbell, T. D.; Shine, R. A.; Title, A. M.; Nagata, S. Bibcode: 2008A&A...481L...9I Altcode: Context: Net circular polarization (NCP) of spectral lines in sunspots has been most successfully explained by the presense of discontinuities in the magnetic field inclination and flow velocity along the line-of-sight in the geometry of the embedded flux tube model of penumbrae (Δγ-effect).
Aims: The fine scale structure of NCP in a sunspot is examined with special attention paid to spatial relations of the Evershed flow to confirm the validity of the present interpretation of the NCP of sunspots.
Methods: High resolution spectro-polarimetric data of a positive-polarity sunspot obtained by the Solar Optical Telescope aboard Hinode are analysed.
Results: A positive NCP is associated with the Evershed flow channels in both limb-side and disk center-side penumbrae and with upflows in the penumbra at disk center. The negative NCP in the disk center-side penumbra is generated in inter-Evershed flow channels.
Conclusions: The first result is apparently inconsistent with the current explanation of NCP with the Δγ-effect but rather suggests a positive correlation between the magnetic field strength and the flow velocity as the cause of the NCP. The second result serves as strong evidence for the presence of gas flows in inter-Evershed flow channels. Title: Hinode SOT Observations of Solar Quiescent Prominence Dynamics Authors: Berger, Thomas E.; Shine, Richard A.; Slater, Gregory L.; Tarbell, Theodore D.; Title, Alan M.; Okamoto, Takenori J.; Ichimoto, Kiyoshi; Katsukawa, Yukio; Suematsu, Yoshinori; Tsuneta, Saku; Lites, Bruce W.; Shimizu, Toshifumi Bibcode: 2008ApJ...676L..89B Altcode: We report findings from multihour 0.2'' resolution movies of solar quiescent prominences (QPs) observed with the Solar Optical Telescope (SOT) on the Hinode satellite. The observations verify previous findings of filamentary downflows and vortices in QPs. SOT observations also verify large-scale transverse oscillations in QPs, with periods of 20-40 minutes and amplitudes of 2-5 Mm. The upward propagation speed of several waves is found to be ~10 km s-1, comparable to the sound speed of a 10,000 K plasma, implying that the waves are magnetoacoustic in origin. Most significantly, Hinode SOT observations reveal that dark, episodic upflows are common in QPs. The upflows are 170-700 km in width, exhibit turbulent flow, and rise with approximately constant speeds of ~20 km s-1 from the base of the prominence to heights of ~10-20 Mm. The upflows are visible in both the Ca II H-line and Hα bandpasses of SOT. The new flows are seen in about half of the QPs observed by SOT to date. The dark upflows resemble buoyant starting plumes in both their velocity profile and flow structure. We discuss thermal and magnetic mechanisms as possible causes of the plumes. Title: Emergence of a Helical Flux Rope under an Active Region Prominence Authors: Okamoto, Takenori J.; Tsuneta, Saku; Lites, Bruce W.; Kubo, Masahito; Yokoyama, Takaaki; Berger, Thomas E.; Ichimoto, Kiyoshi; Katsukawa, Yukio; Nagata, Shin'ichi; Shibata, Kazunari; Shimizu, Toshifumi; Shine, Richard A.; Suematsu, Yoshinori; Tarbell, Theodore D.; Title, Alan M. Bibcode: 2008ApJ...673L.215O Altcode: 2008arXiv0801.1956O Continuous observations were obtained of NOAA AR 10953 with the Solar Optical Telescope (SOT) on board the Hinode satellite from 2007 April 28 to May 9. A prominence was located over the polarity inversion line (PIL) to the southeast of the main sunspot. These observations provided us with a time series of vector magnetic fields on the photosphere under the prominence. We found four features: (1) The abutting opposite-polarity regions on the two sides along the PIL first grew laterally in size and then narrowed. (2) These abutting regions contained vertically weak but horizontally strong magnetic fields. (3) The orientations of the horizontal magnetic fields along the PIL on the photosphere gradually changed with time from a normal-polarity configuration to an inverse-polarity one. (4) The horizontal magnetic field region was blueshifted. These indicate that helical flux rope was emerging from below the photosphere into the corona along the PIL under the preexisting prominence. We suggest that this supply of a helical magnetic flux to the corona is associated with evolution and maintenance of active region prominences. Title: The Horizontal Magnetic Flux of the Quiet-Sun Internetwork as Observed with the Hinode Spectro-Polarimeter Authors: Lites, B. W.; Kubo, M.; Socas-Navarro, H.; Berger, T.; Frank, Z.; Shine, R.; Tarbell, T.; Title, A.; Ichimoto, K.; Katsukawa, Y.; Tsuneta, S.; Suematsu, Y.; Shimizu, T.; Nagata, S. Bibcode: 2008ApJ...672.1237L Altcode: Observations of very quiet Sun using the Solar Optical Telescope/Spectro-Polarimeter (SOT/SP) aboard the Hinode spacecraft reveal that the quiet internetwork regions are pervaded by horizontal magnetic flux. The spatial average horizontal apparent flux density derived from wavelength-integrated measures of Zeeman-induced linear polarization is BTapp = 55 Mx cm -2, as compared to the corresponding average vertical apparent flux density of | BLapp| = 11 Mx cm -2. Distributions of apparent flux density are presented. Magnetic fields are organized on mesogranular scales, with both horizontal and vertical fields showing "voids" of reduced flux density of a few granules spatial extent. The vertical fields are concentrated in the intergranular lanes, whereas the stronger horizontal fields are somewhat separated spatially from the vertical fields and occur most commonly at the edges of the bright granules. High-S/N observations from disk center to the limb help to constrain possible causes of the apparent imbalance between | BLapp| and BTapp, with unresolved structures of linear dimension on the surface smaller by at least a factor of 2 relative to the SOT/SP angular resolution being one likely cause of this discrepancy. Other scenarios for explaining this imbalance are discussed. The horizontal fields are likely the source of the "seething" fields of the quiet Sun discovered by Harvey et al. The horizontal fields may also contribute to the "hidden" turbulent flux suggested by studies involving Hanle effect depolarization of scattered radiation. Title: Hinode Observations of Flux Emergence in Quiet and Active Regions Authors: Lites, B. W.; Centeno, R.; Kubo, M.; Socas-Navarro, H. Berger, T.; Frank, Z.; Shine, R.; Tarbell, T.; Title, A.; Ichimoto, K.; Katsukawa, Y.; Tsuneta, S.; Suematsu, Y.; Shimizu, T.; Nagata, S. Bibcode: 2008ASPC..383...71L Altcode: We review briefly the observational understanding of emergence of flux in both the quiet Sun and active regions in the light of first results from the joint Japan/US/UK Hinode mission. That spacecraft is now providing us with our first continuous, high resolution measurements of the photospheric vector magnetic field, along with high resolution observations of the thermal and dynamic properties of the chromosphere and corona. This review is intended to present a few very early results and to highlight the potential for discovery offered by this extraordinary new mission. The discovery of ubiquitous horizontal magnetic flux in the quiet internetwork regions is presented. Title: Mangetic field properties at the footpoints of solar microflares (active-region transient brightenings) Authors: Shimizu, T.; Kano, R.; Katsukawa, Y.; Kubo, M.; Deluca, E.; Ichimoto, K.; Lites, B.; Nagata, S.; Sakao, T.; Shine, R.; Suematsu, Y.; Tarbell, T.; Title, A.; Tsuneta, S. Bibcode: 2007AGUFMSH52C..06S Altcode: Solar active regions produce numerous numbers of small-scale explosive energy releases, i.e., microflares, which are captured by imaging observations in soft X-rays as transient brightenings of small-scale coronal loops. Thanks to advanced performance of X-Ray Telescope (XRT) onboard the Hinode satellite, we can investigate finer structure of the brightening X-ray sources in more details than we did with Yohkoh data. One of important questions on microflares is what causes microflares. The simultaneous visible-light observations by the Solar Optical Telescope (SOT) allow us to explore magnetic activities and magnetic field configuration at the photospheric footpoints of brightening loops, giving key observations to investigate the question. For our investigations of corona-photosphere magnetic coupling, we have established co-alignment between SOT and XRT with accuracy better than 1 arcsec (Shimizu et al. 2007, PASJ in press). It turns out that Ca II H observations are very useful to identify the exact positions of footpoints of X-ray transient brightening loops. Small "Kernels" are sometimes observed in Ca II H and they may be signature of highly accelerated non-thermal particles impinging on chromosphere. As already shown in Shimizu et al.(2002), frequent transient brightenings are observed at the locations where emerging activities are on going. However, another type of brightening triggering mechanism should exist to explain some observed multiple-loop brightenings. In the multiple-loop brightenings, multiple loops are magnetically in parallel with each other and no apparent magnetic activities, such as emerging and canceling, are observed at and near the footpoints. This paper will present SOT observations of some microflares observed with XRT. Title: Small-Scale Jetlike Features in Penumbral Chromospheres Authors: Katsukawa, Y.; Berger, T. E.; Ichimoto, K.; Lites, B. W.; Nagata, S.; Shimizu, T.; Shine, R. A.; Suematsu, Y.; Tarbell, T. D.; Title, A. M.; Tsuneta, S. Bibcode: 2007Sci...318.1594K Altcode: We observed fine-scale jetlike features, referred to as penumbral microjets, in chromospheres of sunspot penumbrae. The microjets were identified in image sequences of a sunspot taken through a Ca II H-line filter on the Solar Optical Telescope on board the Japanese solar physics satellite Hinode. The microjets’ small width of 400 kilometers and short duration of less than 1 minute make them difficult to identify in existing observations. The microjets are possibly caused by magnetic reconnection in the complex magnetic configuration in penumbrae and have the potential to heat the corona above a sunspot. Title: Chromospheric Alfvénic Waves Strong Enough to Power the Solar Wind Authors: De Pontieu, B.; McIntosh, S. W.; Carlsson, M.; Hansteen, V. H.; Tarbell, T. D.; Schrijver, C. J.; Title, A. M.; Shine, R. A.; Tsuneta, S.; Katsukawa, Y.; Ichimoto, K.; Suematsu, Y.; Shimizu, T.; Nagata, S. Bibcode: 2007Sci...318.1574D Altcode: Alfvén waves have been invoked as a possible mechanism for the heating of the Sun's outer atmosphere, or corona, to millions of degrees and for the acceleration of the solar wind to hundreds of kilometers per second. However, Alfvén waves of sufficient strength have not been unambiguously observed in the solar atmosphere. We used images of high temporal and spatial resolution obtained with the Solar Optical Telescope onboard the Japanese Hinode satellite to reveal that the chromosphere, the region sandwiched between the solar surface and the corona, is permeated by Alfvén waves with strong amplitudes on the order of 10 to 25 kilometers per second and periods of 100 to 500 seconds. Estimates of the energy flux carried by these waves and comparisons with advanced radiative magnetohydrodynamic simulations indicate that such Alfvén waves are energetic enough to accelerate the solar wind and possibly to heat the quiet corona. Title: Magnetic and Doppler Observations of the Photosphere and Low Chromosphere with the Solar Optical Telescope on Hinode Authors: Tarbell, T. D.; Lites, B. W.; Shine, R. A.; Ichimoto, K. Bibcode: 2007AGUFMSH53A1064T Altcode: We present magnetic field and Doppler shift measurements in the Mg I b line at 517.3 nm obtained with the Solar Optical Telescope's Narrowband Filter Imager on Hinode. The line core forms in the low chromosphere, and the wings where the measurements are made probably form around the temperature minimum. Stokes IQUV images in the red and blue wings are combined to make movies of longitudinal magnetograms and Dopplergrams. The direction of the transverse field component is also measurable in strong field concentrations. These are compared with very accurate photospheric magnetic measurements in Fe I 630.2 nm from the Spectro-Polarimeter. This comparison calibrates the filter longitudinal magnetograms in flux density and shows changes in field geometry with height. The Doppler measurements are calibrated using wavelength scans through the Mg line profile. A number of emerging and canceling magnetic features were observed in AR 10961 during its disk passage in late June and early July. Since these were made during the Hinode eclipse season, the observations have somewhat lower spatial resolution than usual (0.32 arcsecond pixels), but the uniformity and sensitivity are excellent. Intermittent upflows seen between canceling magnetic features are interpreted in terms of reconnection outflows. Strong, persistent downflows are seen adjacent to but not on flux concentrations outside of sunspots and pores. In the sunspot, running penumbral waves are clearly visible, and steady downflows are observed over the light bridges. Hinode is a Japanese mission developed and launched by ISAS/ JAXA, with NAOJ as domestic partner and NASA and STFC (UK) as international partners. It is operated by these agencies in cooperation with ESA and NSC (Norway). Title: Chromospheric Anemone Jets as Evidence of Ubiquitous Reconnection Authors: Shibata, Kazunari; Nakamura, Tahei; Matsumoto, Takuma; Otsuji, Kenichi; Okamoto, Takenori J.; Nishizuka, Naoto; Kawate, Tomoko; Watanabe, Hiroko; Nagata, Shin'ichi; UeNo, Satoru; Kitai, Reizaburo; Nozawa, Satoshi; Tsuneta, Saku; Suematsu, Yoshinori; Ichimoto, Kiyoshi; Shimizu, Toshifumi; Katsukawa, Yukio; Tarbell, Theodore D.; Berger, Thomas E.; Lites, Bruce W.; Shine, Richard A.; Title, Alan M. Bibcode: 2007Sci...318.1591S Altcode: 2008arXiv0810.3974S The heating of the solar chromosphere and corona is a long-standing puzzle in solar physics. Hinode observations show the ubiquitous presence of chromospheric anemone jets outside sunspots in active regions. They are typically 3 to 7 arc seconds = 2000 to 5000 kilometers long and 0.2 to 0.4 arc second = 150 to 300 kilometers wide, and their velocity is 10 to 20 kilometers per second. These small jets have an inverted Y-shape, similar to the shape of x-ray anemone jets in the corona. These features imply that magnetic reconnection similar to that in the corona is occurring at a much smaller spatial scale throughout the chromosphere and suggest that the heating of the solar chromosphere and corona may be related to small-scale ubiquitous reconnection. Title: Twisting Motions of Sunspot Penumbral Filaments Authors: Ichimoto, K.; Suematsu, Y.; Tsuneta, S.; Katsukawa, Y.; Shimizu, T.; Shine, R. A.; Tarbell, T. D.; Title, A. M.; Lites, B. W.; Kubo, M.; Nagata, S. Bibcode: 2007Sci...318.1597I Altcode: The penumbra of a sunspot is composed of numerous thin, radially extended, bright and dark filaments carrying outward gas flows (the Evershed flow). Using high-resolution images obtained by the Solar Optical Telescope aboard the solar physics satellite Hinode, we discovered a number of penumbral bright filaments revealing twisting motions about their axes. These twisting motions are observed only in penumbrae located in the direction perpendicular to the symmetry line connecting the sunspot center and the solar disk center, and the direction of the twist (that is, lateral motions of intensity fluctuation across filaments) is always from limb side to disk-center side. Thus, the twisting feature is not an actual twist or turn of filaments but a manifestation of dynamics of penumbral filaments with three-dimensional radiative transfer effects. Title: Hinode SOT observations of plume upflows and cascading downflows in quiescent solar prominences Authors: Berger, T.; Shine, R.; Slater, G.; Tarbell, T.; Title, A.; Lites, B.; Tsuneta, S.; Okamoto, T. J.; Ichimoto, K.; Katsukawa, Y.; Sekii, T.; Suematsu, Y.; Shimizu, T. Bibcode: 2007AGUFMSH53A1065B Altcode: We present several Hinode SOT filtergram movies of quiescent solar prominences that show newly discovered "plume-like" upflows and cascading "waterfall-like" downflows that persist for the entire multi-hour duration of the observations. The flow speeds are on the order of 10 km/sec with typical widths of 400-700 km. Preliminary calculations show that if the upflows are buoyancy driven, the associated thermal perturbation is on the order of 10,000 K, sufficient to explain the dark appearance of the upflows in the interference filter passbands. In addition we observe rotational vortices and body oscillations within the prominences. These new observations challenge current magnetostatic models of solar prominences by showing that prominence plasmas are in constant motion, often in directions perpendicular to the magnetic field lines proposed by the models. TRACE, Hinode/EIS, and Hinode/XRT observations are used to investigate the differential topology of the flows across temperature regimes. Title: Coronal Transverse Magnetohydrodynamic Waves in a Solar Prominence Authors: Okamoto, T. J.; Tsuneta, S.; Berger, T. E.; Ichimoto, K.; Katsukawa, Y.; Lites, B. W.; Nagata, S.; Shibata, K.; Shimizu, T.; Shine, R. A.; Suematsu, Y.; Tarbell, T. D.; Title, A. M. Bibcode: 2007Sci...318.1577O Altcode: 2008arXiv0801.1958O Solar prominences are cool 104 kelvin plasma clouds supported in the surrounding 106 kelvin coronal plasma by as-yet-undetermined mechanisms. Observations from Hinode show fine-scale threadlike structures oscillating in the plane of the sky with periods of several minutes. We suggest that these represent Alfvén waves propagating on coronal magnetic field lines and that these may play a role in heating the corona. Title: Quiet-Sun Internetwork Magnetic Fields from the Inversion of Hinode Measurements Authors: Orozco Suárez, D.; Bellot Rubio, L. R.; del Toro Iniesta, J. C.; Tsuneta, S.; Lites, B. W.; Ichimoto, K.; Katsukawa, Y.; Nagata, S.; Shimizu, T.; Shine, R. A.; Suematsu, Y.; Tarbell, T. D.; Title, A. M. Bibcode: 2007ApJ...670L..61O Altcode: 2007arXiv0710.1405O We analyze Fe I 630 nm observations of the quiet Sun at disk center taken with the spectropolarimeter of the Solar Optical Telescope aboard the Hinode satellite. A significant fraction of the scanned area, including granules, turns out to be covered by magnetic fields. We derive field strength and inclination probability density functions from a Milne-Eddington inversion of the observed Stokes profiles. They show that the internetwork consists of very inclined, hG fields. As expected, network areas exhibit a predominance of kG field concentrations. The high spatial resolution of Hinode's spectropolarimetric measurements brings to an agreement the results obtained from the analysis of visible and near-infrared lines. Title: Center-to-Limb Variation of Stokes V Asymmetries in Solar Pores Observed with the Hinode Spectro-Polarimeter Authors: Morinaga, Shuji; Nagata, Shin'ichi; Ichimoto, Kiyoshi; Suematsu, Yoshinori; Tsuneta, Saku; Katsukawa, Yukio; Shimizu, Toshifumi; Shine, Richard A.; Tarbell, Theodore D.; Title, Alan M.; Lites, Bruce; Kubo, Masahito; Sakurai, Takashi Bibcode: 2007PASJ...59S.613M Altcode: Here we present spectro-polarimetric measurements of several pores and the surrounding regions taken with the Solar Optical Telescope aboard Hinode at various viewing angles. We analyzed the Stokes V area asymmetry, and confirmed that it is depressed at the center of the pores, while it shows large positive values (a blue lobe larger than a red lobe) in the surrounding area; this is consistent with a previous report. In addition to this ring of positive asymmetry, we found regions of alternating positive and negative area asymmetries when weak V regions were observed near the solar limb. The positive asymmetry occurs on the disk-center side and the negative asymmetry on the limb side of the magnetic concentrations. These center-to-limb variations of the Stokes V area asymmetry can be interpreted as being a systematic inflow of plasma into the magnetic concentrations from their surroundings. Title: Initial Results on Line-of-Sight Field Calibrations of SP/NFI Data Taken by SOT/Hinode Authors: Chae, Jongchul; Moon, Yong-Jae; Park, Young-Deuk; Ichimoto, Kiyoshi; Sakurai, Takashi; Suematsu, Yoshinori; Tsuneta, Saku; Katsukawa, Yukio; Shimizu, Toshifumi; Shine, Richard A.; Tarbell, Theodore D.; Title, Alan M.; Lites, Bruce; Kubo, Masahito; Nagata, Shin'ichi; Yokoyama, Takaaki Bibcode: 2007PASJ...59S.619C Altcode: We present initial results on the line-of-sight field calibration of the two kinds of Stokes I and V data taken by the Solar Optical Telescope on the satellite Hinode: spectral profiles of Stokes I and V parameters recorded on the Spectro-polarimeter (SP), and monochromatic images of the same parameters recorded on the Narrow-band Filter Imager (NFI). By applying the center-of-gravity method to the SP data of AR10930 taken on 2006 December 11, we determined the line-of-sight field at every location in the active region. As a result, we found that the line-of-sight field strength ranges up to 2kG in plages, even without taking into account the filling factor, and up to 3.5kG or higher values inside the umbra of the major sunspot. We calibrated the NFI data in reference to the field determined from the SP data. In regions outside the sunspots and the penumbral regions, we adopted a linear relation, B|| = βV / I, between the circular polarization, V / I, and the line-of-sight field strength, B||, and obtained β = 23.5kG in regions outside the sunspots, and β = 12.0kG in penumbral regions. In umbral regions of sunspots, a first-order polynomial was adopted to model the reversal of the polarization signal over the field strength. Title: Response of the Solar Atmosphere to Magnetic Flux Emergence from Hinode Observations Authors: Li, Hui; Sakurai, Takashi; Ichimito, Kiyoshi; Suematsu, Yoshinori; Tsuneta, Saku; Katsukawa, Yukio; Shimizu, Toshifumi; Shine, Richard A.; Tarbell, Theodore D.; Title, Alan M.; Lites, Bruce; Kubo, Masahito; Nagata, Shin'ichi; Kotoku, Jun; Shibasaki, Kiyoto; Saar, Steven H.; Bobra, Monica Bibcode: 2007PASJ...59S.643L Altcode: No abstract at ADS Title: Initial Helioseismic Observations by Hinode/SOT Authors: Sekii, Takashi; Kosovichev, Alexander G.; Zhao, Junwei; Tsuneta, Saku; Shibahashi, Hiromoto; Berger, Thomas E.; Ichimoto, Kiyoshi; Katsukawa, Yukio; Lites, Bruce; Nagata, Shin'ichi; Shimizu, Toshifumi; Shine, Richard A.; Suematsu, Yoshinori; Tarbell, Theodore D.; Title, Alan M. Bibcode: 2007PASJ...59S.637S Altcode: 2007arXiv0709.1806S Results from initial helioseismic observations by the Solar Optical Telescope on-board Hinode are reported. It has been demonstrated that intensity oscillation data from the Broadband Filter Imager can be used for various helioseismic analyses. The k - ω power spectra, as well as the corresponding time-distance cross-correlation function, which promise high-resolution time-distance analysis below the 6-Mm travelling distance, were obtained for G-band and CaII-H data. Subsurface supergranular patterns were observed from our first time-distance analysis. The results show that the solar oscillation spectrum is extended to much higher frequencies and wavenumbers, and the time-distance diagram is extended to much shorter travel distances and times than were observed before, thus revealing great potential for high-resolution helioseismic observations from Hinode. Title: Hinode Observations of Horizontal Quiet Sun Magnetic Flux and the ``Hidden Turbulent Magnetic Flux'' Authors: Lites, Bruce; Socas-Navarro, Hector; Kubo, Masahito; Berger, Thomas; Frank, Zoe; Shine, Richard A.; Tarbell, Theodore D.; Title, Alan M.; Ichimoto, Kiyoshi; Katsukawa, Yukio; Tsuneta, Saku; Suematsu, Yoshinori; Shimizu, Toshifumi Bibcode: 2007PASJ...59S.571L Altcode: We present observations of magnetic fields of the very quiet Sun near disk center using the Spectro-Polarimeter of the Solar Optical Telescope aboard the Hinode satellite. These observations reveal for the first time the ubiquitous presence of horizontal magnetic fields in the internetwork regions. The horizontal fields are spatially distinct from the vertical fields, demonstrating that they are not arising mainly from buffeting of vertical flux tubes by the granular convection. The horizontal component has an average ``apparent flux density'' of 55Mxcm-2 (assuming the horizontal field structures are spatially resolved), in contrast to the average apparent vertical flux density of 11Mxcm-2. The vertical fields reside mainly in the intergranular lanes, whereas the horizontal fields occur mainly over the bright granules, with a preference to be near the outside edge of the bright granules. The large apparent imbalance of vertical and horizontal flux densities is discussed, and several scenarios are presented to explain this imbalance. Title: Strategy for the Inversion of Hinode Spectropolarimetric Measurements in the Quiet Sun Authors: Orozco Suárez, David; Bellot Rubio, Luis R.; Del Toro Iniesta, Jose Carlos; Tsuneta, Saku; Lites, Bruce; Ichimoto, Kiyoshi; Katsukawa, Yukio; Nagata, Shin'ichi; Shimizu, Toshifumi; Shine, Richard A.; Suematsu, Yoshinori; Tarbell, Theodore D.; Title, Alan M. Bibcode: 2007PASJ...59S.837O Altcode: 2007arXiv0709.2033O In this paper we propose an inversion strategy for the analysis of spectropolarimetric measurements taken by Hinode in the quiet Sun. The Spectro-Polarimeter of the Solar Optical Telescope aboard Hinode records the Stokes spectra of the FeI line pair at 630.2nm with unprecendented angular resolution, high spectral resolution, and high sensitivity. We discuss the need to consider a local stray-light contamination to account for the effects of telescope diffraction. The strategy is applied to observations of a wide quiet Sun area at disk center. Using these data we examine the influence of noise and initial guess models in the inversion results. Our analysis yields the distributions of magnetic field strengths and stray-light factors. They show that quiet Sun internetwork regions consist mainly of hG fields with stray-light contamination of about 0.8. Title: Hinode Calibration for Precise Image Co-Alignment between SOT and XRT (2006 November-2007 April) Authors: Shimizu, Toshifumi; Katsukawa, Yukio; Matsuzaki, Keiichi; Ichimoto, Kiyoshi; Kano, Ryohei; Deluca, Edward E.; Lundquist, Loraine L.; Weber, Mark; Tarbell, Theodore D.; Shine, Richard A.; Sôma, Mitsuru; Tsuneta, Saku; Sakao, Taro; Minesugi, Kenji Bibcode: 2007PASJ...59S.845S Altcode: 2007arXiv0709.4098S To understand the physical mechanisms for activity and heating in the solar atmosphere, the magnetic coupling from the photosphere to the corona is an important piece of information from the Hinode observations, and therefore precise positional alignment is required among the data acquired by different telescopes. The Hinode spacecraft and its onboard telescopes were developed to allow us to investigate magnetic coupling with co-alignment accuracy better than 1". Using the Mercury transit observed on 2006 November 8 and co-alignment measurements regularly performed on a weekly basis, we have determined the information necessary for precise image co-alignment, and have confirmed that co-alignment better than 1" can be realized between Solar Optical Telescope (SOT) and X-Ray Telescope (XRT) with our baseline co-alignment method. This paper presents results from the calibration for precise co-alignment of CCD images from SOT and XRT. Title: Hinode Observations of a Vector Magnetic Field Change Associated with a Flare on 2006 December 13 Authors: Kubo, Masahito; Yokoyama, Takaaki; Katsukawa, Yukio; Lites, Bruce; Tsuneta, Saku; Suematsu, Yoshinori; Ichimoto, Kiyoshi; Shimizu, Toshifumi; Nagata, Shin'ichi; Tarbell, Theodore D.; Shine, Richard A.; Title, Alan M.; Elmore David Bibcode: 2007PASJ...59S.779K Altcode: 2007arXiv0709.2397K Continuous observations of the flare productive active region 10930 were successfully carried out with the Solar Optical Telescope aboard the Hinode spacecraft during 2006 December 6 to 19. We focused on the evolution of photospheric magnetic fields in this active region, and the magnetic field properties at the site of the X3.4 class flare, using a time series of vector field maps with high spatial resolution. The X3.4 class flare occurred on 2006 December 13 at the apparent collision site between the large, opposite polarity umbrae. Elongated magnetic structures with alternatingly positive and negative polarities resulting from flux emergence appeared one day before the flare in the collision site penumbra. Subsequently, the polarity inversion line at the collision site became very complicated. The number of bright loops in CaII H increased during the formation of these elongated magnetic structures. Flare ribbons and bright loops evolved along the polarity inversion line and one footpoint of the bright loop was located in a region having a large departure of the field azimuth angle with respect to its surroundings. SOT observations with high spatial resolution and high polarization precision revealed temporal change in the fine structure of magnetic fields at the flare site: some parts of the complicated polarity inversion line then disappeared, and in those regions the azimuth angle of the photospheric magnetic field changed by about 90°, becoming more spatially uniform within the collision site. Title: Fine-Scale Structures of the Evershed Effect Observed by the Solar Optical Telescope aboard Hinode Authors: Ichimoto, Kiyoshi; Shine, Richard A.; Lites, Bruce; Kubo, Masahito; Shimizu, Toshifumi; Suematsu, Yoshinori; Tsuneta, Saku; Katsukawa, Yukio; Tarbell, Theodore D.; Title, Alan M.; Nagata, Shin'ichi; Yokoyama, Takaaki; Shimojo, Masumi Bibcode: 2007PASJ...59S.593I Altcode: The small-scale structure of the Evershed effect is being studied using data obtained by the Spectropolarimeter and the Broadband Filter Imager of the Solar Optical Telescope aboard Hinode. We find that the Evershed flow starts at the leading edge of inwardly migrating bright penumbral grains, and turns to nearly a horizontal flow preferentially in the dark lanes of the penumbra. A number of small elongated regions that have an upward motion of ∼ 1kms-1 are found in the deep photosphere distributed over the penumbra. They are cospatial with bright grains and have relatively horizontal magnetic fields. A number of patches having a strong downward motion associated with the opposite magnetic polarity from the sunspot are also found in the mid and outer penumbra. They could be identified as foot points of the Evershed flow channels, though the identification of individual pairs is not straightforward. Our results provide strong support for some recent findings from ground-based high-resolution observations, and are in general agreement with the well-known picture of the uncombed structure of the penumbra, in which the penumbrae consist of rising flux tubes carrying nearly horizontal Evershed flows embedded in more vertical background magnetic fields. Title: Flare Ribbons Observed with G-band and FeI 6302Å, Filters of the Solar Optical Telescope on Board Hinode Authors: Isobe, Hiroaki; Kubo, Masahito; Minoshima, Takashi; Ichimoto, Kiyoshi; Katsukawa, Yukio; Tarbell, Theodore D.; Tsuneta, Saku; Berger, Thomas E.; Lites, Bruce; Nagata, Shin'ichi; Shimizu, Toshifumi; Shine, Richard A.; Suematsu, Yoshinori; Title, Alan M. Bibcode: 2007PASJ...59S.807I Altcode: 2007arXiv0711.3946I The Solar Optical Telescope (SOT) on board the Hinode satellite observed an X3.4 class flare on 2006 December 13. A typical two-ribbon structure was observed, not only in the chromospheric CaII H line, but also in the G-band and FeI 6302Å line. The high-resolution, seeing-free images achieved by SOT revealed, for the first time, sub-arcsec fine structures of the ``white light'' flare. The G-band flare ribbons on sunspot umbrae showed a sharp leading edge, followed by a diffuse inside, as well as a previously known core-halo structure. The underlying structures, such as umbral dots, penumbral filaments, and granules, were visible in the flare ribbons. Assuming that the sharp leading edge was directly heated by a particle beam and the diffuse parts were heated by radiative back-warming, we estimated the depth of the diffuse flare emission using an intensity profile of the flare ribbon. We found that the depth of the diffuse emission was about 100km or less from the height of the source of radiative back-warming. The flare ribbons were also visible in the Stokes-V images of FeI 6302Å, as a transient polarity reversal. This is probably related to a ``magnetic transient'' reported in the literature. The intensity increase in Stokes-I images indicates that the FeI 6302Å line was significantly deformed by the flare, which may cause such a magnetic transient. Title: Small-Scale Magnetic-Flux Emergence Observed with Hinode Solar Optical Telescope Authors: Otsuji, Kenichi; Shibata, Kazunari; Kitai, Reizaburo; Ueno, Satoru; Nagata, Shin'ichi; Matsumoto, Takuma; Nakamura, Tahei; Watanabe, Hiroko; Tsuneta, Saku; Suematsu, Yoshinori; Ichimoto, Kiyoshi; Shimizu, Toshifumi; Katsukawa, Yukio; Tarbell, Theodore D.; Lites, Bruce; Shine, Richard A.; Title Alan M. Bibcode: 2007PASJ...59S.649O Altcode: 2007arXiv0709.3207O We observed small-scale magnetic-flux emergence in a sunspot moat region by the Solar Optical Telescope (SOT) aboard the Hinode satellite. We analyzed filtergram images observed at wavelengths of Fe 6302Å, G band, and CaII H. In Stokes I images of Fe 6302Å, emerging magnetic flux was recognized as dark lanes. In the G band, they showed to be their shapes almost the same as in Stokes I images. These magnetic fluxes appeared as dark filaments in CaII H images. Stokes V images of Fe 6302Å showed pairs of opposite polarities at footpoints of each filament. These magnetic concentrations were identified to correspond to bright points in G band/CaII H images. From an analysis of time-sliced diagrams, we derived the following properties of emerging flux, which are consistent with those of previous studies: (1) Two footpoints separate each other at a speed of 4.2kms-1 during the initial phase of evolution, and decrease to about 1kms-1 10minutes later. (2) CaII H filaments appear almost simultaneously with the formation of dark lanes in Stokes I in an observational cadence of 2minutes. (3) The lifetime of the dark lanes in the Stokes I and G band is 8minutes, while that of Ca filament is 12minutes. An interesting phenomena was observed, that an emerging flux tube expanded laterally in the photosphere with a speed of 3.8kms-1. A discussion on the horizontal expansion of the flux tube is given with refernce to previous simulation studies. Title: Observations of Sunspot Oscillations in G Band and CaII H Line with Solar Optical Telescope on Hinode Authors: Nagashima, Kaori; Sekii, Takashi; Kosovichev, Alexander G.; Shibahashi, Hiromoto; Tsuneta, Saku; Ichimoto, Kiyoshi; Katsukawa, Yukio; Lites, Bruce; Nagata, Shin'ichi; Shimizu, Toshifumi; Shine, Richard A.; Suematsu, Yoshinori; Tarbell, Theodore D.; Title, Alan M. Bibcode: 2007PASJ...59S.631N Altcode: 2007arXiv0709.0569N Exploiting high-resolution observations made by the Solar Optical Telescope on board Hinode, we investigate the spatial distribution of the power spectral density of the oscillatory signal in and around the active region NOAA 10935. The G-band data show that in the umbra the oscillatory power is suppressed in all frequency ranges. On the other hand, in CaII H intensity maps oscillations in the umbra, so-called umbral flashes, are clearly seen with the power peaking around 5.5mHz. The CaII H power distribution shows the enhanced elements with the spatial scale of the umbral flashes over most of the umbra, but there is a region with suppressed power at the center of the umbra. The origin and property of this node-like feature remain unexplained. Title: Hinode SP Vector Magnetogram of AR10930 and Its Cross-Comparison with MDI Authors: Moon, Yong-Jae; Kim, Yeon-Han; Park, Young-Deuk; Ichimoto, Kiyoshi; Sakurai, Takashi; Chae, Jongchul; Cho, Kyung Suk; Bong, Suchan; Suematsu, Yoshinori; Tsuneta, Saku; Katsukawa, Yukio; Shimojo, Masumi; Shimizu, Toshifumi; Shine, Richard A.; Tarbell, Theodore D.; Title, Alan M.; Lites, Bruce; Kubo, Masahito; Nagata, Shin'ichi; Yokoyama, Takaaki Bibcode: 2007PASJ...59S.625M Altcode: We present one Hinode Spectropolarimeter (SP) magnetogram of AR 10930 that produced several major flares. The inversion from Stokes profiles to magnetic field vectors was made using the standard Milne-Eddington code. We successfully applied the Uniform Shear Method for resolving the 180° ambiguity to the magnetogram. The inversion gave very strong magnetic field strengths (near 4500 gauss) for a small portion of area in the umbra. Considering that the observed V-profile of 6301.5Å was well-fitted as well as a direct estimation of the Zeeman splitting results in 4300-4600 gauss, we think that the field strengths should not be far from the actual value. A cross-comparison of the Hinode SP and SOHO MDI high resolution flux densities shows that the MDI flux density could be significantly underestimated by about a factor of two. In addition, it has a serious negative correlation (the so-called Zeeman saturation effect) with the Hinode SP flux density for umbral regions. Finally, we could successfully obtain a recalibrated MDI magnetogram that has been corrected for the Zeeman saturation effect using not only a pair of MDI intensity and magnetogram data simultaneously observed, but also the relationship from the cross-comparison between the Hinode SP and MDI flux densities. Title: Formation Process of a Light Bridge Revealed with the Hinode Solar Optical Telescope Authors: Katsukawa, Yukio; Yokoyama, Takaaki; Berger, Thomas E.; Ichimoto, Kiyoshi; Kubo, Masahito; Lites, Bruce; Nagata, Shin'ichi; Shimizu, Toshifumi; Shine, Richard A.; Suematsu, Yoshinori; Tarbell, Theodore D.; Title, Alan M.; Tsuneta, Saku Bibcode: 2007PASJ...59S.577K Altcode: 2007arXiv0709.2527K The Solar Optical Telescope (SOT) on-board Hinode successfully and continuously observed the formation process of a light bridge in a matured sunspot of the NOAA active region 10923 for several days with high spatial resolution. During its formation, many umbral dots were observed to be emerging from the leading edges of penumbral filaments, and rapidly intruding into the umbra. The precursor of the light bridge formation was also identified as a relatively slow inward motion of the umbral dots, which emerged not near the penumbra, but inside the umbra. The spectro-polarimeter on SOT provided physical conditions in the photosphere around the umbral dots and the light bridges. We found that the light bridges and the umbral dots had significantly weaker magnetic fields associated with upflows relative to the core of the umbra, which implies that there was hot gas with weak field strength penetrating from the subphotosphere to near the visible surface inside those structures. There needs to be a mechanism to drive the inward motion of the hot gas along the light bridges. We suggest that the emergence and the inward motion are triggered by a buoyant penumbral flux tube as well as subphotospheric flow crossing the sunspot. Title: Umbral Fine Structures in Sunspots Observed with Hinode Solar Optical Telescope Authors: Kitai, Reizaburo; Watanabe, Hiroko; Nakamura, Tahei; Otsuji, Ken-ichi; Matsumoto, Takuma; UeNo, Satoru; Nagata, Shin'ichi; Shibata, Kazunari; Muller, Richard; Ichimoto, Kiyoshi; Tsuneta, Saku; Suematsu, Yoshinori; Katsukawa, Yukio; Shimizu, Toshifumi; Tarbell, Theodore D.; Shine, Richard A.; Title, Alan M.; Lites, Bruce Bibcode: 2007PASJ...59S.585K Altcode: 2007arXiv0711.3266K A high resolution imaging observation of a sunspot umbra was made with the Hinode Solar Optical Telescope. Filtergrams at wavelengths of the blue and green continua were taken during three consecutive days. The umbra consisted of a dark core region, several diffuse components, and numerous umbral dots. We derived basic properties of umbral dots (UDs), especially their temperatures, lifetimes, proper motions, spatial distribution, and morphological evolution. The brightness of UDs is confirmed to depend on the brightness of their surrounding background. Several UDs show fission and fusion. Thanks to the stable condition of the space observation, we could for the first time follow the temporal behavior of these events. The derived properties of the internal structure of the umbra are discussed from the viewpoint of magnetoconvection in a strong magnetic field. Title: Formation of Moving Magnetic Features and Penumbral Magnetic Fields with Hinode/SOT Authors: Kubo, Masahito; Ichimoto, Kiyoshi; Shimizu, Toshifumi; Tsuneta, Saku; Suematsu, Yoshinori; Katsukawa, Yukio; Nagata, Shin'ichi; Tarbell, Theodore D.; Shine, Richard A.; Title, Alan M.; Frank, Zoe A.; Lites, Bruce; Elmore, David Bibcode: 2007PASJ...59S.607K Altcode: 2007arXiv0709.1853K Vector magnetic fields of moving magnetic features (MMFs) were well observed with the Solar Optical Telescope (SOT) aboard the Hinode satellite. We focused on the evolution of three MMFs with the SOT in this study. We found that an MMF having relatively vertical fields with the same polarity as the sunspot was detached from the penumbra around the granules appearing in the outer penumbra. This suggests that granular motions in the outer penumbra are responsible for disintegration of the sunspot. Two MMFs with polarity opposite to the sunspot are located around the outer edge of horizontal fields extending from the penumbra. This is evidence that the MMFs with polarity opposite to the sunspot are the prolongation of penumbral horizontal fields. Redshifts larger than the sonic velocity in the photosphere are detected for some of the MMFs with polarity opposite to the sunspot. Title: A Tale of Two Spicules: The Impact of Spicules on the Magnetic Chromosphere Authors: de Pontieu, Bart; McIntosh, Scott; Hansteen, Viggo H.; Carlsson, Mats; Schrijver, Carolus J.; Tarbell, Theodore D.; Title, Alan M.; Shine, Richard A.; Suematsu, Yoshinori; Tsuneta, Saku; Katsukawa, Yukio; Ichimoto, Kiyoshi; Shimizu, Toshifumi; Nagata, Shin'ichi Bibcode: 2007PASJ...59S.655D Altcode: 2007arXiv0710.2934D We use high-resolution observations of the Sun in CaIIH (3968Å) from the Solar Optical Telescope on Hinode to show that there are at least two types of spicules that dominate the structure of the magnetic solar chromosphere. Both types are tied to the relentless magnetoconvective driving in the photosphere, but have very different dynamic properties. ``Type-I'' spicules are driven by shock waves that form when global oscillations and convective flows leak into the upper atmosphere along magnetic field lines on 3--7minute timescales. ``Type-II'' spicules are much more dynamic: they form rapidly (in ∼ 10s), are very thin (≤ 200 km wide), have lifetimes of 10-150s (at any one height), and seem to be rapidly heated to (at least) transition region temperatures, sending material through the chromosphere at speeds of order 50--150kms-1. The properties of Type II spicules suggest a formation process that is a consequence of magnetic reconnection, typically in the vicinity of magnetic flux concentrations in plage and network. Both types of spicules are observed to carry Alfvén waves with significant amplitudes of order 20kms-1. Title: Hinode Observations of the Onset Stage of a Solar Filament Eruption Authors: Sterling, Alphonse C.; Moore, Ronald L.; Berger, Thomas E.; Bobra, Monica; Davis, John M.; Jibben, Patricia; Kano, Ryohei; Lundquist, Loraine L.; Myers, D.; Narukage, Noriyuki; Sakao, Taro; Shibasaki, Kiyoto; Shine, Richard A.; Tarbell, Theodore D.; Weber, Mark Bibcode: 2007PASJ...59S.823S Altcode: We used Hinode X-Ray Telescope (XRT) and Solar Optical Telescope (SOT) filtergraph (FG) Stokes-V magnetogram observations, to study the early onset of a solar eruption that includes an erupting filament that we observe in TRACE EUV images. The filament undergoes a slow rise for at least 20min prior to its fast eruption and strong soft X-ray (SXR) flaring; such slow rises have been previously reported, and the new Hinode data elucidate the physical processes occurring during this period. XRT images show that during the slow-rise phase, an SXR sigmoid forms from apparent reconnection low in the sheared core field traced by the filament, and there is a low-level intensity peak in both EUV and SXRs during the slow rise. MDI and SOT FG Stokes-V magnetograms show that the pre-eruption filament is along a neutral line between opposing-polarity enhanced network cells, and the SOT magnetograms show that these opposing fields are flowing together and canceling for at least six hours prior to eruption. From the MDI data we measured the canceling network fields to be ∼ 40G, and we estimated that ∼ 1019 Mx of flux canceled during the five hours prior to eruption; this is only ∼ 5% of the total flux spanned by the eruption and flare, but apparently its tether-cutting cancellation was enough to destabilize the sigmoid field holding the filament and resulted in that field's eruption. Title: Performance Characteristics of the Solar-B Spectro-Polarimeter Authors: Lites, B. W.; Elmore, D. F.; Streander, K. V.; Hoffmann, C. M.; Tarbell, T. D.; Title, A. M.; Shine, R. A.; Ichimoto, K.; Tsuneta, S.; Shimizu, T.; Suematsu, Y. Bibcode: 2007ASPC..369...55L Altcode: The Focal Plane Package (FPP) of the Solar Optical Telescope (SOT) includes the first precision Spectro-Polarimeter (SP) for solar space observations. The FPP/SP will provide high precision measures of the vector magnetic field in the solar photosphere. Here we present some as-built performance specifications for the entire system of telescope + polarimeter. The FPP-SP system represents significant gains in several aspects over existing spectro-polarimetric systems; notably, angular resolution, polarimetric accuracy, spectral purity, and most importantly, temporal continuity of stable, high angular resolution. In this short summary of the poster, a few of the performance characteristics of the SP are presented. Title: Calibration of the SOT Polarization Authors: Ichimoto, K.; Suematsu, Y.; Shimizu, T.; Katsukawa, Y.; Noguchi, M.; Nakagiri, M.; Miyashita, M.; Tsuneta, S.; Tarbell, T. D.; Shine, R. A.; Hoffmann, C. M.; Cruz, T.; Lites, B. W.; Elmore, D. F. Bibcode: 2007ASPC..369...39I Altcode: Calibration of SOT polarization property was performed using natural sunlight and well calibrated sheet polarizer (linear and circular) placed on the entrance of the telescope. The polarimeter response matrices were determined for the spectropolarimeter (SP) and the narrowband filter imager (NFI), and it is shown that they are well behave as predicted and constant over the field of view. The crosstalk between I,Q,U,V will be suppressed to the negligible level at the photometric accuracy of 10^{-3} after the calibration with the obtained matrices. The sensitivity of SOT on linear and circular polarizations at each wavelength observed by NFI are also obtained. Title: Calibration of SOT Dopplergrams Authors: Katsukawa, Y.; Ichimoto, K.; Sekii, T.; Suematsu, Y.; Tsuneta, S.; Shine, R. A.; Tarbell, T. D. Bibcode: 2007ASPC..369...43K Altcode: Narrow-band Filter Imager on SOT provides Dopplergrams (DGs) which are images of Doppler (line- of-sight) velocities. Observations with DGs are critically important in studies of photospheric dynamics and helioseismology. The primary photospheric line used for DGs is Fe I 5576 Å which is a line insensitive to Zeeman effect. We made a calibration function for the 5576 Å DGs to get actual Doppler velocities from velocity indexes using an atlas spectrum and simulated transmission profiles for the tunable filter (TF) on SOT. Using data sets taken in the natural sun-light test, we quantitatively evaluated accuracy of the DGs by comparing the rotational speed of the Sun measured with DGs with the expected one. There was a little systematic error in the velocity obtained by SOT, but the error was less than 20 % of the predicted velocities. Title: Vector Spectropolarimetry of Dark-cored Penumbral Filaments with Hinode Authors: Bellot Rubio, L. R.; Tsuneta, S.; Ichimoto, K.; Katsukawa, Y.; Lites, B. W.; Nagata, S.; Shimizu, T.; Shine, R. A.; Suematsu, Y.; Tarbell, T. D.; Title, A. M.; del Toro Iniesta, J. C. Bibcode: 2007ApJ...668L..91B Altcode: 2007arXiv0708.2791B We present spectropolarimetric measurements of dark-cored penumbral filaments taken with Hinode at a resolution of 0.3". Our observations demonstrate that dark-cored filaments are more prominent in polarized light than in continuum intensity. Far from disk center, the Stokes profiles emerging from these structures are very asymmetric and show evidence for magnetic fields of different inclinations along the line of sight, together with strong Evershed flows of at least 6-7 km s-1. In sunspots closer to disk center, dark-cored penumbral filaments exhibit regular Stokes profiles with little asymmetries due to the vanishing line-of-sight component of the horizontal Evershed flow. An inversion of the observed spectra indicates that the magnetic field is weaker and more inclined in the dark cores as compared with the surrounding bright structures. This is compatible with the idea that dark-cored filaments are the manifestation of flux tubes carrying hot Evershed flows. Title: Emergence of Small-Scale Magnetic Loops in the Quiet-Sun Internetwork Authors: Centeno, R.; Socas-Navarro, H.; Lites, B.; Kubo, M.; Frank, Z.; Shine, R.; Tarbell, T.; Title, A.; Ichimoto, K.; Tsuneta, S.; Katsukawa, Y.; Suematsu, Y.; Shimizu, T.; Nagata, S. Bibcode: 2007ApJ...666L.137C Altcode: 2007arXiv0708.0844C We study the emergence of magnetic flux at very small spatial scales (less than 2") in the quiet-Sun internetwork. To this aim, a time series of spectropolarimetric maps was taken at disk center using the instrument SP/SOT on board Hinode. The LTE inversion of the full Stokes vector measured in the Fe I 6301 and 6302 Å lines allows us to retrieve the magnetic flux and topology in the region of study. In the example presented here, the magnetic flux emerges within a granular structure. The horizontal magnetic field appears prior to any significant amount of vertical field. As time goes on, the traces of the horizontal field disappear, while the vertical dipoles drift-carried by the plasma motions-toward the surrounding intergranular lanes. These events take place within typical granulation timescales. Title: Chromospheric Micro-jets Discovered Above Sunspot Penumbrae Authors: Katsukawa, Yukio; Tsuneta, S.; Suematsu, Y.; Ichimoto, K.; Shimizu, T.; Kubo, M.; Nagata, S.; Berger, T.; Tarbell, T.; Shine, R.; Title, A. Bibcode: 2007AAS...210.9413K Altcode: 2007BAAS...39..219K The Solar Optical Telescope (SOT) aboard HINODE allows us to observe dynamical activities in the solar photosphere and the chromosphere with high and stable image quality of 0.2 arcseconds. This superior performance of SOT provides new findings of fine-scale transient activities occurring in the chromosphere. In this paper, we report discovery of fine-scale jet-like phenomena ubiquitously observed above sunspot penumbrae. The jets are identified in image sequences of a sunspot taken through a Ca II H line filter at 3968A. The Ca II H line is sensitive to about 10^4 K plasma in the chromosphere.

Their length is typically between 3000 and 10000km, and their width is smaller than 500km. It is notable that their lifetime is shorter than 1 minute. Those small spatial and temporal scale possibly makes it difficult to identify the phenomena in existing ground-based observations. The jets are easily identified when a sunspot is located far from the disk center, and motion of the bright features suggests that mass is erupted from lower chromosphere to upper atmosphere. Velocities of the motion are estimated to be 50 to 100 km/s from their lateral motion of intensity patterns. The velocities are much faster than sound speeds in the chromosphere. A possible cause of such high-speed jets is magnetic reconnection at the lower chromosphere resulted from fluted magnetic configuration in penumbrae which is suggested by vector magnetic field measurements in the photosphere. Title: Magnetic Patches in Internetwork Quiet Sun Authors: De Wijn, Alfred; Lites, B.; Berger, T.; Shine, R.; Title, A.; Katsukawa, Y.; Tsuneta, S.; Suematsu, Y.; Shimizu, T.; Hinode Team Bibcode: 2007AAS...210.9412D Altcode: 2007BAAS...39Q.219D We study strong flux elements in the quiet sun in the context of the nature of quiet-sun magnetism, its coupling to chromospheric, transition-region and coronal fields, and the nature of a local turbulent dynamo. Strong, kilogauss flux elements show up intermittently as small bright points in G-band and Ca II H images. Although bright points have been extensively studied in the magnetic network, internetwork magnetism has only come under scrutiny in recent years. A full spectrum of field strengths seems to be ubiquitously present in the internetwork at small spatial scales, with the stronger elements residing in intergranular lanes. De Wijn et al. (2005) found that bright points in quiet sun internetwork areas appear recurrently with varying intensity and horizontal motion within long-lived patches that outline cell patterns on mesogranular scales. They estimate that the "magnetic patches" have a mean lifetime of nine hours, much longer than granular timescales. We use multi-hour sequences of G-band and Ca II H images as well as magnetograms recorded by the Hinode satellite to follow up on their results. The larger field of view, the longer sequences, the addition of magnetograms, and the absence of atmospheric seeing allows us to better constrain the patch lifetime, to provide much improved statistics on IBP lifetime, to compare IBPs to network bright points, and to study field polarity of IBPs in patches and between nearby patches.

Hinode is an international project supported by JAXA, NASA, PPARC and ESA. We are grateful to the Hinode team for all their efforts in the design, build and operation of the mission. Title: High Resolution Observation of Spicules in Ca II H with Hinode/SOT Authors: Suematsu, Yoshinori; Katsukawa, Y.; Ichimoto, K.; Tsuneta, S.; Okamoto, T.; Nagata, S.; Shimizu, T.; Tarbell, T.; Shine, R.; Title, A. Bibcode: 2007AAS...210.9411S Altcode: 2007BAAS...39..219S High cadence observation with a Ca II H broadband filtergraph (passband of 0.25 nm) of the Solar Optical Telescope (SOT) aboard HINODE has revealed dynamical nature of solar limb spicules. Thanks to a diffraction-limited and low-scattered light property of the instrument, we can track the detailed evolution of individual spicules for the first time with a spatial resolution of 0.2 arcsec. The spicules in Ca II H are typically several arcsec tall and have multi-thread structure; each threads are a few tenth of arcsec wide. It should be stressed that most spicules do not show a simple up-and-down motion along a rigid path line. They start with bright structure emanating from Ca II H bright region, get widen and diffused with time and ascent, showing expansion with lateral or even helical motion in tall events. Small and short lived spicules tend to fade out after ascent. We will present new findings of spicule dynamics in different magnetic environments and discuss about long standing controversy of its motion and evolution. Title: Hinode/SOT Observation of Fine Structure of the Evershed Flow Authors: Ichimoto, Kiyoshi; Suematsu, Y.; Tsuneta, S.; Katsukawa, Y.; Shimojo, M.; Kubo, M.; Shimizu, T.; Shine, R.; Tarbell, T.; Title, A.; Lites, B.; Elmore, D.; Yokoyama, T.; Nagaka, S. Bibcode: 2007AAS...210.9408I Altcode: 2007BAAS...39..218I Small scale structure of the Evershed effect was studied using the Spectropolarimeter (SP) and Broadband Filter Imager (BFI) of SOT aboard Hinode. SP maps and high cadence continuum images of BFI coverting entire sunspots are used to investigate the spatial distribution of the flow field, brightness and magnetic fields. It is revealed that the Evershed flow starts at the front edge of inwardly migrating penumbral grains with an upward velocity component and turns to nearly holizontal flow preferentially in dark lanes (or dark core of filaments) of the penumbra. Our results are in general agreement with the well known uncombed penumbral concept in which the Evershed flow takes place in nearly holizontal field channels. We discovered a number of tiny elongated regions in deep photosphere in which there is an obvious upward motion of 1-1.5km/s distributing over the penumbra.

They could be identified as the 'foot points' of the individual Evershed flow channels. Cross-correlation among the flow speed, intensity, magnetic field strength and inclination, and distribution of string down flows in and around the penumbra will also be discussed. Title: Magnetic Flux Emergence In The Quiet Sun Photosphere Authors: Centeno, Rebecca; Lites, B.; Socas-Navarro, H.; Frank, Z.; Shine, R.; Tarbell, T.; Title, A.; Ichimoto, K.; Tsuneta, S.; Katsukawa, Y.; Suematsu, Y.; Kubo, M.; Shimizu, T. Bibcode: 2007AAS...210.9406C Altcode: 2007BAAS...39..218C We study the emergence of magnetic flux at very small spacial scales (less than 1 arcsec) in the quiet Sun internetwork. To this aim, several time series of spectropolarimetric maps were taken at disk center using the instrument SP/SOT on board Hinode. The LTE inversion of the full Stokes vector measured in the Fe I 6301 and 6302 lines will allow us to retrieve the magnetic flux and topology in the region of study. We find that the magnetic flux emerges typically within the granular structures. In many cases, the horizontal magnetic field appears prior to any significant amount of vertical field. As time goes on, the traces of the horizontal field dissapear while the the vertical dipoles drift -carried by the plasma motions- towards the surrounding intergranular lanes. Sometimes they stay trapped there for a while but they eventually either disappear by disgregation/cancelation or agregate to other magnetic field concentrations giving rise to larger flux elements. The time scale of these events is of the order of 10-20 minutes. Title: Formation of Moving Magnetic Features and Penumbral Magnetic Fields Authors: Kubo, Masahito; Ichimoto, K.; Shimizu, T.; Tsuneta, S.; Suematsu, Y.; Katsukawa, Y.; Nagata, S.; Lites, B. W.; Frank, Z.; Tarbell, T. D.; Shine, R. A.; Title, A. M. Bibcode: 2007AAS...210.9410K Altcode: 2007BAAS...39..218K We investigate the formation process of Moving Magnetic Features (MMFs) observed with Hinode/SOT. Moving magnetic features are small magnetic elements moving outward in the moat region surrounding mature sunspots. We derive vector magnetic fields of MMFs around simple sunspots near the disk center. Most of MMFs with polarity opposite to the sunspot have large redshift around the penumbral outer boundary. We find that some of them have Doppler velocities of about 10 km/s and such large Doppler motion is observed only in the Stokes V profile. The Stokes Q and U profiles in the same pixel do not have any significant Doppler motions. Horizontal magnetic fields of the penumbra frequently extend to the moat region and the MMFs having horizontal fields with polarity same as the sunspot are formed. The MMFs with polarity opposite to the sunspot appear around the outer edge of the extending penumbral fields. We also find penumbral spines, which have more vertical magnetic fields than the surroundings, branch off at their outer edge and MMFs having relatively vertical fields with polarity same as the sunspot are detached from the outer edge of the branch. The branch of penumbral spine is formed when granular cells in the moat region go into the penumbra. Title: Ubiquitous Horizontal Magnetic Fields in the Quiet Solar Photosphere as Revealed by HINODE Meaurements Authors: Lites, Bruce W.; Socas Navarro, H.; Berger, T.; Frank, Z.; Shine, R.; Tarbell, T.; Title, A.; Ichimoto, K.; Katsukawa, Y.; Tsuneta, S.; Suematsu, Y.; Kubo, M.; Shimizu, T.; Nagata, S.; Hinode Team Bibcode: 2007AAS...210.6303L Altcode: 2007BAAS...39..171L Measurements with the HINODE Spectro-Polarimeter (SP) of the quiet Sun allow characterization of the weak, mixed-polarity magnetic flux at the highest angular resolution to date (0.3"), and with good polarimetric sensitivity(0.025% relative to the continuum). The image stabilization of the HINODE spacecraft allows long integrations with degradation of the image quality only by the evolution of the solar granulation. From the Stokes V profile measurements we find an average solar "Apparent Flux Density" of 14 Mx cm-2, with significant Stokes V signals at every position on the disk at all times. However, there are patches of meso-granular size (5-15") where the flux is very weak. At this high sensitivity, transverse fields produce measurable Stokes Q,U linear polarization signals over a majority of the area, with apparent transverse flux densities in the internetwork significantly larger than the corresponding longitudinal flux densities. When viewed at the center of the solar disk, the Stokes V signals (longitudinal fields) show a preference for occurrence in the intergranular lanes, and the Q,U signals occur preferably over the granule interiors, but neither association is exclusive.

Hinode is an international project supported by JAXA, NASA, PPARC and ESA. We are grateful to the Hinode team for all their efforts in the design, build and operation of the mission. Title: Discovery Of Cool Cloud-like Structures In The Corona With Hinode Solar Optical Telescope Authors: Okamoto, Takenori; Tsuneta, S.; Katsukawa, Y.; Ichimoto, K.; Suematsu, Y.; Shimizu, T.; Nagata, S.; Shibata, K.; Tarbell, T.; Shine, R.; Berger, T.; Lites, B.; Myers, D. Bibcode: 2007AAS...210.9426O Altcode: 2007BAAS...39..221O A solar observation satellite Hinode (Japanese for sun rise) was launched in September 2006.Hinode carried 3 advanced solar telescopes, visible light telescope, EUV imaging spectrometer, and X-ray telescope to simultaneously observe the photosphere, chromosphere, transition region, and corona. In the performance verification phase of the Hinode spacecraft with its telescopes, we observed an active region AR10921 near the west limb of the solar disk on November 9 2006. At this point, we planned to observe spicules on the limb with a broadband filter dedicated to Ca II H line (3968A). Ca II-H emission line (3968A) comes from plasma with temperature of approx. 10(4) K, which is much lower than the coronal temperature of 10(6-7) K. In addition to spectacular spicules, we find a large cloud-like structure located 10,000-20,000 km above the limb. The cloud has a very complex fine structure with dominant horizontal thread-like structure. Some features are moving horizontally and also have clear vertical oscillatory motions. The periods and amplitudes of these oscillations are 130-250 seconds and 200-850 km, respectively. The vertical oscillatory motion sometimes has a coherence length as long as 16,000 km. We conclude that from various observational features this vertical oscillation is a signature of Alfven waves propagating along the horizontal magnetic fields. We will discuss their origin and implications. Title: Hinode/SOT Observations of Sunspot Penumbral Dynamics and Evolution Authors: Shine, Richard A.; Hagenaar, M.; Tarbell, T.; Title, A.; Lites, B.; Ichimoto, K.; Tsuneta, S.; Katsakawa, Y.; Suematsu, Y.; Nagata, S.; Kubo, M.; Shimizu, T. Bibcode: 2007AAS...210.9407S Altcode: 2007BAAS...39..218S The Solar Optical Telescope (SOT) on the Hinode satellite (launched October 2006) has obtained long and nearly continuous time series of several large sunspots including those in NOAA AR's 10923, 10925, and 10930. Here we use high resolution movies taken primarily with the broad band Ca II (396.8nm) and G band (430.5nm) channels and magnetograms taken with the 630.2nm narrow band channel to study the details and short term evolution of penumbral fine structures as well as the long term evolution of the sunspots. We compute flow maps and use space/time slices to track motions of Evershed clouds, penumbral grains, and visualize oscillations. The data contain examples of penumbral formation and disintegration including "orphan" penumbra (i.e., penumbra without an obvious umbra). There is also an interesting instance of "colliding" penumbra in AR 10930 as two sunspots of opposite polarity converged. The zone of apparent shear was associated with several flares.

This work was supported by NASA contract NNM07AA01C Title: Magnetic Field Diagnostic Capability of Solar-B/SOT: Filtergraph Instrument Authors: Ichimoto, K.; Suematsu, Y.; Shimizu, T.; Katsukawa, Y.; Tsuneta, S.; Tarbell, T. D.; Shine, R. A.; Hoffmann, C. M.; Title, A. M.; Lites, B. W.; Elmore, D. F.; Streander, K. V. Bibcode: 2006ASPC..358..189I Altcode: The Narrowband Filter Instrument (NFI) of the Solar Optical Telescope onboard Solar-B provides 2D magnetograms/Dopplergrams with a tunable Lyot filter (width ∼ 0.1 Å) in 6 selected wavelength bands, and spatial sampling of 0.08 arcsec/px. The Zeeman-effect sensitivity of NFI and the detection limits of weak magnetic fields are evaluated for 2 photospheric and 3 chromospheric lines. Magnetic-field retrievability from the NFI observables is studied using synthetic Stokes profiles of Fe I 5250 Å. We find that, with optimized wavelength sampling at 4 positions, the inferred magnetic field is sufficiently accurate under the hypothesis of constant magnetic field and velocity along the LOS. Title: Moving Magnetic Features Observed Simultaneously With Trace And DST Authors: Hagenaar-Daggett, Hermance J.; Shine, R. A. Bibcode: 2006SPD....37.0709H Altcode: 2006BAAS...38..229H In this paper, we study observations of sunspots made in June - July 2005, with TRACE 1600A and the Dunn Solar telescope at Sac Peak. In that period MDI was in a continuous contact mode in which it makes only FD magnetograms. The 1600A line, however, is highly correlated with the unsigned magnetic flux density, and we use an automated algorithm to detect moving magnetic features around sunspots. We compare our findings with the ground based observations in the Gband, CaK line, Halpha, and Stokes spectra. Title: Coupling effects throughout the solar atmosphere: Emerging magnetic flux and structure formation Authors: Ryutova, M.; Shine, R. Bibcode: 2006JGRA..111.3101R Altcode: 2006JGRA..11103101R We report observations of the "birth," formation, and evolution of compact coronal structures associated with strong localized motions generated by emerging magnetic flux in the photosphere. We use multiwavelength time series of data taken simultaneously with the Swedish Vacuum Solar Telescope (SVST) on La Palma, the TRACE satellite, and the MDI instrument on SOHO. We find that long before the magnetic pore is formed, the chromosphere and transition region show a high activity above the future site of pore formation: rising but not yet visible magnetic flux exerts a strong pressure on the overlying plasma generating highly collimated plasma flows seen in the Hα images. About the time when the magnetic pores are formed and the Hα surges bifurcate into the established arc-like flows, a system of compact coronal loops is formed, showing direct connection between the motions associated with the evolving magnetic fields and the coronal structure formation. We propose a mechanism that may lead to the observed phenomena based on the generation of currents by strong disturbances propagating upward from a limited surface area. Title: Moving Magnetic Features around Sunspots Authors: Hagenaar, Hermance J.; Shine, Richard A. Bibcode: 2005ApJ...635..659H Altcode: We study statistical properties of small-scale magnetic features around sunspots using time sequences of high-resolution magnetograms of eight sunspots made with the Michelson Doppler Imager (MDI) on board SOHO. Flow maps around the spots are also derived from cross-correlation analysis of MDI continuum or TRACE white light and used for comparison of photospheric flow patterns with the tracks of moving magnetic features. An automated algorithm to find and track unipolar concentrations of magnetic field was developed. Depending on the velocity, size, and distance from the spot, a selected subset of all concentrations can be identified as moving magnetic features (MMFs). Our method finds 4-24 MMFs per hour around the spots, with higher counts for larger sunspots. After being first detected, the MMFs have an average flux content <Φ0>=2.5×1018 Mx. Their average lifetime is about 1 hr, but it takes a concentration only tmax=25 minutes to reach its maximum flux content of about <Φmax>=6.1×1018 Mx. MMFs are found to transport a net flux out of a spot at a rate of (0.4-6.2)×1019 Mx hr-1: if sunspots were to decay only by outflowing MMFs, it would take a sunspot of 1022 Mx one to several weeks to completely disassemble. The MMFs have an initial velocity of 0>=1.8 km s-1, faster than the average moat flow. Before merging into the moat region or surrounding network, they travel a distance <Δ>=3.5 Mm. The tracks of the individual MMFs correlate with the direction of local plasma flows and sometimes display a spokelike pattern around the sunspots. We find an average initial size 0>=1.7 Mm2, but the distribution of sizes suggests features with a diameter of only 600-1000 km, which would not be recognized by our algorithm. Comparison of a cotemporal, cospatial magnetogram made with the Swedish Vacuum Solar Telescope (SVST) on La Palma (with 12 times the spatial resolution) indicates that unipolar magnetic fluxes in the MDI magnetogram may be comprised of smaller elements with both polarities. Title: Calibration and Tesing of the Tunable Filter on Solar B Authors: Shine, R. A.; Title, A. M.; Tarbell, T. D.; Mitchell, K.; Tavarez, L.; Rosenberg, W. Bibcode: 2005AGUSMSP43A..04S Altcode: The tunable filter in the Focal Plane Package (FPP) on the Japanese Solar B satellite, scheduled for launch in August 2006, was designed, built, and tested at the Lockheed Martin Advanced Technology Center (LMATC). It is an eight element wide field calcite filter (an improved Lyot type) with a spectral resolution of about 100mÅ and a tuning range of 11.87Å at 6302Å. Using 6 prefilters, it operates in bands covering the 5172Å Fe I, 5250Å Fe I, 5576Å Fe I, 5896Å Na I, 6302Å Fe I, and 6563Å H I lines. Here we describe the testing and calibrations used to determine the tuning parameters as functions of temperature and wavelength for the six bands. We also measure performance using sunlight and laser sources in a standalone mode and integrated into the FPP package. Images and derived magnetograms and Dopplergrams using a low resolution solar image have also been obtained while attached to the Solar B telescope and using a heliostat at the LMATC in Palo Alto. In the course of this work we have also refined the mathematical description for these types of filters, especially the error terms that arise from residual misalignments. In particular, we now believe we understand the intensity oscillations seen in this and earlier Lyot tunable filters. Title: Dynamics and Properties of Supergranulation from TRACE Observations Authors: Simon, G. W.; Shine, R. A. Bibcode: 2004AAS...204.3718S Altcode: 2004BAAS...36..712S Using a unique set of white-light images taken by the Transition Region and Corona Explorer (TRACE) satellite over a 7 day period in April 2000, we investigate the properties and evolution of supergranulation. A 384x384 arcsec area of the solar photosphere was observed as it rotated from Stonyhurst longitude 45E to 45W. Granulation is well defined in these images which were taken at a 60s cadence for most of the 7 days. Hence we are able to use local correlation tracking (LCT) with sufficient spatial and temporal resolution to track both mesogranules and supergranules. Improved techniques for LCT are discussed and compared.

Divergence and other parameters derived from flow maps are used to identify and accurately trace supergranular boundaries and tessellate the image areas into distinct supergranules as well as smaller areas with less coherent flow patterns. We have used these to derive sizes, lifetimes, and other properties of supergranules. Motivated by recent work of Rast, Lisle, and Toomre (2004), and Lisle, Rast, and Toomre (2004), we also present results comparing the rotational rate of the supergranular and mesogranular patterns and N/S alignments of these features.

This work was supported by NASA contract NAS5-38099, the Air Force Research Laboratory, and the National Solar Observatory. Title: Response of the Corona to Magnetic Activity in Underlying Plage Regions Authors: Ryutova, M.; Shine, R. Bibcode: 2004ApJ...606..571R Altcode: We study the response of the solar corona to magnetic activity in the underlying plage regions using high-resolution Michelson Doppler Imager magnetograms co-aligned with multiwavelength images taken by TRACE at chromospheric and coronal temperatures. We show that the EUV emission above plage regions that are dominated by single-polarity magnetic elements always has an amorphous shape that topologically mimics the shape of the underlying plage. Spacetime slices of the amorphous emission in the coronal lines show coherent braidlike structures with almost constant period for a given area. Contrary to this, coronal emission above mixed-polarity plages is highly discrete and consists of sporadic localized radiative transients. As different regions of strongly inhomogeneous corona evolve in different ways, separate mechanisms for energy production, flow, and release are probably required. We argue that in all cases the primary energy source lies in continuous hydromagnetic activity among the photospheric magnetic fields. The character of this activity determines the processes of the extraction of energy and its transport throughout the solar atmosphere. We propose a physical mechanism that may explain the diverse properties of the UV/EUV emission in upper layers of atmosphere and its relevance to the photospheric magnetic fields. Title: Magnetic Coupling Between the Solar Surface and Corona: Theory and Observations Authors: Ryutova, Margarita; Shine, Richard Bibcode: 2004AIPC..703..203R Altcode: Multi-wavelength observations taken simultaneously by several instruments on the Solar and Heliospheric Observatory (SOHO) and Transition Region and Coronal Explorer (TRACE) revealed a clear connection between the photospheric magnetic fields and the energetic events in the overlying atmosphere. We find that the EUV coronal emission above the photosphere dominated by single polarity magnetic elements is spongy in space and has coherent braid-like structures in time. Contrary to these long living structures, corona above the regions with mixed polarity magnetic elements is highly discrete and consists of sporadic microflares, supersonic jets and their combinations. We believe that in the unipolar magnetic regions the energy flow from the surface to corona is associated with the nonlinear collective phenomena in the ensemble of oscillating magnetic flux tubes. These phenomena lead to formation of hot coronal ``clouds'' that have the properties of energetically open turbulence with tendency to self-organization. Jets and microflares above the mixed polarity regions are associated with shock waves produced by reconnecting magnetic flux tubes in the photosphere and subsequent interaction of shocks which leads to hydrodynamic cumulation of energy, which leads to impulsive phenomena similar to shaped charges. Title: Moving Magnet Features around Sunspots Authors: Hagenaar, H. J.; Shine, R. A. Bibcode: 2003AGUFMSH42B0544H Altcode: Moving magnetic features (MMF's) associated with small-scale emerging fluxes near the sunspot penumbra are believed to play an important role in mass and energy flow near sunspots. Since their discovery 30 year ago, only a few theoretical interpretations have been proposed on the real identity of MMF's: they may be associated with field lines detached from a decaying spot, or with closed magnetic loops. MMF's have remained a difficult subject for observations, requiring high spatial resolution movies for at least several hours. Coronal emission does not show immediate response to the birth and disappearance of individual MMF's; and the role of MMF's in the dynamics of upper layers of the atmosphere remains unclear. We present the results of recent, multi-wavelength observations designed to study the dynamics of MMF's from the time of their emergence to the moment when they merge into network or moat. Vector magnetograms made with the Dunn Telescope at Sunspot, NM, are co-aligned with MDI magnetograms, and TRACE 1600 Å and Fe IX/X 171 Å images, showing field orientation at the site of emergence, and the response of the chromosphere and corona to dynamic changes in the MMF's. These data allow meaningful statistics on MMF's and their relation to sunspot evolution. Title: Observations of Rotating Sunspots from TRACE Authors: Brown, D. S.; Nightingale, R. W.; Alexander, D.; Schrijver, C. J.; Metcalf, T. R.; Shine, R. A.; Title, A. M.; Wolfson, C. J. Bibcode: 2003SoPh..216...79B Altcode: Recent observations from TRACE in the photospheric white-light channel have shown sunspots that rotate up to 200° about their umbral centre over a period of 3-5 days. The corresponding loops in the coronal fan are often seen to twist and can erupt as flares. In an ongoing study, seven cases of rotating sunspots have been identified, two of which can be associated with sigmoid structures appearing in Yohkoh/SXT and six with events seen by GOES. This paper analyzes the rotation rates of the sunspots using TRACE white-light data. Observations from AR 9114 are presented in detail in the main text and a summary of the results for the remaining six sunspots is presented in Appendixes A-F. Discussion of the key results, particularly common features, are presented, as well as possible mechanisms for sunspot rotation. Title: Interaction and Dynamics of the Photospheric Network Magnetic Elements Authors: Ryutova, M.; Tarbell, T. D.; Shine, R. Bibcode: 2003SoPh..213..231R Altcode: Small-scale magnetic elements in the quiet photospheric network are believed to play a key role in the energy flow from the solar surface to upper layers of atmosphere. Their intense hydro-magnetic activity includes merging and fragmentation of same polarity fluxes, `total' or partial cancellation of neighboring flux elements of opposite polarity, dynamic appearance and disappearance of compact bipoles, etc. We study the general features of these processes, and show that non-collinearity of flux tubes, sharp stratification of low atmosphere and finite plasma beta lead to several specific effects in the interacting flux tubes that may explain the morphological properties of network magnetic field and also provide a mechanism for the energy build up and release in the nearby chromosphere and transition region. We show that during the collision of flux tubes in the photosphere reconnection occurs regardless of whether the flux tubes are of opposite or of the same polarity. But the dynamics of reconnection products are significantly different and lead to different macroscopic effects that can be observed. Title: Close Correlation among Hα Surges, Magnetic Flux Cancellations, and UV Brightenings Found at the Edge of an Emerging Flux Region Authors: Yoshimura, Keiji; Kurokawa, Hiroki; Shimojo, Masumi; Shine, Richard Bibcode: 2003PASJ...55..313Y Altcode: Surge activities were observed at the edge of an emerging flux region. We studied the relations between the features around the surges in various data sets: magnetogram, Hα, G-band, UV, EUV, and soft X-rays. We showed that the surge activities in Hα and the brightenings in TRACE 1600Å images correlate well in both time and space with the cancellation of magnetic fluxes around an emerging flux region. In particular, at the onset of surge activity, a close correlation among them was clearly found. These facts are consistent with the magnetic reconnection model. The released energy through magnetic reconnection, which is estimated to be 1028 erg, is sufficiently large to produce surge activities. No prominent brightenings were observed in soft X-ray and EUV images during the surge activities. This may suggest that the energy releases occurred at a layer of high densities. Title: Visualizing and Interpreting Very High Resolution Solar Movies Authors: Shine, R. A.; Hurlburt, N.; Title, A. M.; Nightingale, R. W. Bibcode: 2002AGUFMSH52A0498S Altcode: Benefiting from advances in detector technology, image compression, and data storage capacities, current and upcoming solar instruments, especially the Solar Dynamics Observatory (SDO) due to be launched in 2007, will produce immense amounts of data in the form of movies with individual images in the 2048x2048 (4 Mpixel) to 4096x4096 (16 Mpixel) range. This is beyond the capability of most contemporary computer or video displays but several are now becoming available. In order to develop concepts and software for working with existing and future data sets, we have been working with a 9 Mpixel IBM T221 LCD display driven by an SGI Octane 2 workstation. This is a desktop display with a 22 inch diagonal screen. We will demonstrate our prototype system using several combinations of movies from the Swedish Vacuum Solar Tower (SVST) at La Palma, and the TRACE and SOHO satellites and discuss some approaches for the more challenging SDO data products. Title: High Speed Reconnection in the Low Corona Authors: Title, A. M.; Shine, R. A.; Schrijver, C. J. Bibcode: 2002AGUFMSH52A0470T Altcode: High cadence observations taken with the Transition Region and Corona Explorer (TRACE) instrument in the 1600Å\ band (with ≈~2 second cadence) and in the Fe~IX/X 171Å\ band (≈~8 seconds cadence) reveal fast reconnection events of several types. The most common is a newly emerging magnetic loop that reconnects with an overlying fan of loops. As the loops intersect, material is injected into the overlying loops. A newly formed small bright condensation travels in a helical path with a pitch angle of about 45 degrees and a speed of 700 to 1000 km/s. Movies of example events in both spectral bands will be shown. This work was supported by NASA contract NAS5-38099. Title: Estimating the Effects of JPEG Compression and Radiation on the Accuracy of Vector Magnetic Fields Measurements for Solar-B Authors: Lites, B.; Shine, R. A.; López Ariste, A.; Tarbell, T. D. Bibcode: 2002AGUFMSH52A0471L Altcode: The Japanese Solar-B satellite, currently scheduled for launch in September 2005, includes a spectro-polarimeter (SP) to precisely measure the full Stokes polarization vector (I,Q,U,V) in the Fe I lines at 6302Å. These will be processed to produce vector magnetograms of the solar surface using algorithms based on those for the Advanced Stokes Polarimeter (ASP) as described in Skumanich, et al, 1997, ApJ Suppl 110. Accumulations of the raw images into time averaged I,Q,U,V images will be done on board and the results will be 12 bit JPEG compressed to make the best use of the available telemetry. Hence a single radiation hit in a raw image affects the entire time average at that point. Also, radiation spikes affect JPEG compression performance. Because of concerns about these effects, we simulated them separately and in combination using ASP data and radiation level measurements from the TRACE satellite. Like TRACE, Solar-B will fly in a high inclination, sun synchronous orbit and be exposed to radiation from the polar radiation belts as well as the SAA. Since the SP detector will be better shielded than that on TRACE, we hope that these will be an over estimate of the effects. The results from the simulations are very encouraging. We find that for active region magnetic fields we can use JPEG to compress the data volume by more than a factor of 10 without compromising the accuracy of the inferred magnetic field vector. The radiation in the polar regions has little effect and even the much stronger SAA radiation causes average perturbations that are less than the formal errors for sunspot fields and about twice the formal errors for plage fields. However, very weak field measurements will benefit from less lossy compression and periods of low radiation. Of course, the very strong radiation hits always produce artifacts. Compression performance is affected only slightly so it will not be necessary to avoid observations in the SAA because of excessive telemetry usage. This work was supported by NASA contract NAS8-01002. Title: TRACE, SOHO/EIT, and SOHO/MDI Observations of AR0030, Including Rotating Sunspots and the July 15, 2002 X3.0 Flare in Ultraviolet and Extreme Ultraviolet Authors: Nightingale, R. W.; Shine, R. A.; Alexander, D.; Freeland, S. L.; Frank, Z. A.; Brown, D. S. Bibcode: 2002AGUFMSH52A0467N Altcode: On July 15, 2002 TRACE and several SOHO instruments observed an X3.0 flare in AR0030 near 2000 UT. During this period TRACE was primarily observing in its 1600Å ultraviolet (UV) channel (most sensitive to temperatures around 100,000 K in the flare). The 195Å extreme ultraviolet (EUV) channel of SOHO/EIT (which is most sensitive to about 1.6 MK) will be utilized in this poster, in addition to the magnetic field measurements of SOHO/MDI during this event period. TRACE followed the active region for over 10 days, starting about 4 days before the flare. Broadband white light TRACE images of the photosphere indicate that one or more of the sunspots were rotating, a possible precursor to the flare. Images and movies of AR0030 in the various wavelengths will be shown. The flare region was so intense in the TRACE UV that it is very difficult to show both the quiescent and flaring regions, so the UV movie will focus on the flaring plasma with its 2 eruptions. In the EIT EUV, more coronal structure away from the flare can be seen. Analysis of the rotational rates of the sunspots will be given along with their possible coupling to the flare. This work was supported by NASA under contract NAS5-38099. Title: Observations of rotating sunspots and their effect in the corona Authors: Brown, D. S.; Nightingale, R. W.; Alexander, D.; Schrijver, C. J.; Metcalf, T. R.; Shine, R. A.; Title, A. M.; Wolfson, C. J. Bibcode: 2002ESASP.505..261B Altcode: 2002IAUCo.188..261B; 2002solm.conf..261B Recent observations from TRACE have seen sunspots, in the photospheric white light filter, rotate up to 180 degrees about their umbral centre. The corresponding loops in the coronal fan are seen to twist and can erupt. In an ongoing study, five cases of rotating sunspots have been identified, three of which can be identified with sigmoid structures appearing in Yohkoh/SXT. This paper will present images from one of these events, showing the coupling between the photosphere and the corona, and observational analysis deducing the rotation speeds and how they change through time and with radius of the sunspot. In particular, the paper will focus on the best example of a rotating sunspot observed so far, that of AR 9114 which occurred over 8-10 August 2000 and was observed by TRACE, SoHO/MDI and Yohkoh/SXT. The sunspot rotated 150 degrees within this time and is associated with a sigmoid. Title: Photospheric Magnetic Activities Responsible for Soft X-Ray Pointlike Microflares. I. Identifications of Associated Photospheric/Chromospheric Activities Authors: Shimizu, T.; Shine, R. A.; Title, A. M.; Tarbell, T. D.; Frank, Z. Bibcode: 2002ApJ...574.1074S Altcode: By combining Yohkoh soft X-ray images with high-resolution magnetograms simultaneously obtained at La Palma, we studied photospheric magnetic signatures responsible for soft X-ray microflares (active-region transient brightenings). In order to have a reliable correspondence between the photosphere and the corona, we studied 16 pointlike transient brightenings with X-ray source size less than 10" occurring during periods when the seeing was excellent at La Palma, although a lot of transient brightenings were in forms of multiple- or single-loop structures. In half of the studied events, small-scale emergences of magnetic flux loops are found in the vicinity of the transient brightenings. Six events of that half show that a small-scale flux emergence accompanies the X-ray brightening 5-30 minutes prior to its onset. In the other half of the studied events, no apparent evolutionary change of magnetic flux elements is found associated with the transient brightenings. Many of these events are found in rather strong magnetic fields, such as sunspots and pores, implying that small-scale changes of magnetic flux are obscured or suppressed by strong magnetic fields. The horizontal plasma flows derived from local cross-correlation tracking of granules in continuum images are suppressed at the feet of some X-ray transient brightenings. Title: Concurrent Rotating Sunspots, Twisted Coronal Fans, Simgoid Structures and Coronal Mass Ejections Authors: Nightingale, R. W.; Brown, D. S.; Metcalf, T. R.; Schrijver, C. J.; Shine, R. A.; Title, A. M.; Wolfson, C. J. Bibcode: 2002mwoc.conf..149N Altcode: In an on-going study, several sunspots, in apparent rotation, have been identified in TRACE photospheric white light (WL) images with accompanying twisting of coronal fans in the corresponding EUV (171, 195 AA) images. These observations can also be temporally and spatially associated with S or inverse-S shaped regions (sigmoid structures) appearing in Yohkoh SXT images and with concurrent coronal mass ejections (CMEs) and/or flares. We have determined the rotational speed of the apparently rotating sunspot in AR 9114 over 8-10 August 2000, established the inverse S shape observed in the SXT data, and viewed a rapid, bright flash of possible reconnection in a TRACE EUV movie. A CME was observed during the 15-18 August 1999 event, which also included an inverse S shaped region in the SXT data, and a rotating sunspot and twisting coronal fans in the TRACE data. The large Bastille Day CME event of 14 July 2000 was accompanied by one or more apparently rotating sunspots as observed in TRACE WL and by an inverse S shaped region as seen in a difference SXT image. Movies and plots of some of these data will be shown along with flow maps and a list of the pertinent parameters for several rotating sunspots. We will report on our attempt to determine the vertical electric current flowing through the 8 August 2000 sunspot utilizing the Mees vector magnetograph data in order to better understand the apparent rotation "driver". These observations display the coupling of the solar magnetic field from the photosphere into the corona. Title: Pre-Flare Heating Around the Temperature Minimum Region Found Right Prior to an X-Class Flare Authors: Kurokawa, H.; Ishii, T. T.; Wang, T. J.; Shine, R. Bibcode: 2002mwoc.conf..257K Altcode: Studies of magnetic shear developments and pre-flare activities in flare-productive sunspot regions are fundamentally important for the study of flare energy build-up and energy release mechanism. Several previous works demonstrated that the emergence of a twisted magnetic flux rope, which is originally formed in the convection zone, must be the source of the strong magnetic shear development in a sunspot region to produce a strong flare activity (Kurokawa 1987, Tanaka 1991, Ishii et al. 2000). We are still, however, far from sufficiently understanding how the twisted structures of a magnetic flux rope is formed in the convection zone, and where and how such a twisted magnetic rope untwists and releases its energy as flaresNULL A flare productive active region NOAA 9026, which showed an interesting evolution during a coordinated observation between the Domeless Solar Telescope of Hida Observatory, Swedish Telescope of La Palma, and TRACE Satellite from 3 through 12 June of 2000, provided us a rare opportunity to study a new important aspect of a twisted magnetic flux rope and its rapidly-untwisted motions to have caused strong flares. From the analyses of the evolution of this region, we first found a clear evidence of pre-flare heating or energy release from the upper photosphere through the lower chromosphere from about two hours before the energy release in the corona as an X-class flare. We suggest that this pre-flare energy release in the lower atmosphere is closely related to the emergence of the twisted magnetic flux rope from below the photosphere. Title: Surges, Magnetic Flux Cancellations, and UV Brightenings around an Emerging Flux Region Authors: Yoshimura, K.; Kurokawa, H.; Shimojo, M.; Shine, R. Bibcode: 2002mwoc.conf...99Y Altcode: Surge activities, which are observed in Hα images, have been studying for a long time. Many authors noticed that cancellations of magnetic flux was an important factor for surge activities and proposed the models based on magnetic reconnection. But there are not many observations which have enough cadence for comparison changes of magnetic field with surge activities. So the correlation between surges and magnetic flux cancellations is not clear yet. (ex. Zhang et al. 2001) We studied the temporal and spatial relations between surge activities and other phenomena which may be accompanied by surge activities. The data we used here are from coordinated observation with Swedish Vacuum Solar Telescope on La Palma, TRACE and SOHO/MDI. So high cadence images for the same target are available in various wavelengths. MDI, for example, took magnetogram data every one minutes with high resolution mode at that time. The main results from this study are as follows: (1) We can not find any large time lag between the onset of the surge and of the magnetic fields cancellation. This is a conflict result against the one in Zhang et al. (2) There were UV brightenings which correlated well with rapid cancellation of magnetic fields. (3) The UV brightenings located just on neutral lines with some displacement from the region where rapid magnetic cancellation occurred. These observational fact can be explained by magnetic reconnection model. Title: Dynamics of the solar chromosphere. III. Ultraviolet brightness oscillations from TRACE Authors: Krijger, J. M.; Rutten, R. J.; Lites, B. W.; Straus, Th.; Shine, R. A.; Tarbell, T. D. Bibcode: 2001A&A...379.1052K Altcode: We analyze oscillations in the solar atmosphere using image sequences from the Transition Region and Coronal Explorer (TRACE) in three ultraviolet passbands which sample the upper solar photosphere and low chromosphere. We exploit the absence of atmospheric seeing in TRACE data to furnish comprehensive Fourier diagnostics (amplitude maps, phase-difference spectra, spatio-temporal decomposition) for quiet-Sun network and internetwork areas with excellent sampling statistics. Comparison displays from the ground-based Ca Ii H spectrometry that was numerically reproduced by Carlsson & Stein are added to link our results to the acoustic shock dynamics in this simulation. The TRACE image sequences confirm the dichotomy in oscillatory behaviour between network and internetwork and show upward propagation above the cutoff frequency, the onset of acoustic shock formation in the upper photosphere, phase-difference contrast between pseudo-mode ridges and the interridge background, enhanced three-minute modulation aureoles around network patches, a persistent low-intensity background pattern largely made up of internal gravity waves, ubiquitous magnetic flashers, and low-lying magnetic canopies with much low-frequency modulation. The spatio-temporal occurrence pattern of internetwork grains is found to be dominated by acoustic and gravity wave interference. We find no sign of the high-frequency sound waves that have been proposed to heat the quiet chromosphere, but such measurement is hampered by non-simultaneous imaging in different passbands. We also find no signature of particular low-frequency fluxtube waves that have been proposed to heat the network. However, internal gravity waves may play a role in their excitation. Title: Flow Map Studies of Supergranule and Mesogranule Evolution from TRACE Authors: Shine, R. A.; Frank, Z. A.; Tarbell, T. D.; Simon, G. W. Bibcode: 2001AGUFMSH11A0702S Altcode: From 00:44 UT 22-April-2000 to 00:09 UT 29-April-2000 we obtained a nearly continuous set of white light images using the Transition Region and Corona Explorer (TRACE) satellite. A 384x384 arc second field of view was used that tracked solar rotation from Stonyhurst longitudes 45E to 45W along the solar equator. The total time is nearly 7 days with images taken every minute over most of the interval. The largest temporal gap was 45m and there were only 9 gaps longer than 10m. The area was mostly free of active regions. These images are broad band white light with 0.5 arc second pixels. Granulation is well defined and we used local correlation techniques (LCT) to compute flow maps of the horizontal velocities with a resolution of about 5 arc seconds. The flow map resolution and quality suffer somewhat near the longitude extrema but the maps are usable throughout the 7 days to define supergranules and mesogranules. We compute horizontal divergence to study the motions of mesogranules and the evolution and lifetime of supergranules. When enough telemetry capacity was available, we also obtained co-spatial images in the TRACE Fe IX/X 171Å channel and the 1600Å channel. We use these to study the response of the corona and chromosphere to the photospheric motions. During times with particularly high telemetry throughput, we took white light images every 30 seconds. This allows us to empirically determine the noise in our flow maps using two interleaved and disjoint sets of white light data, each with one minute intervals. This work was supported by NASA contract NAS5-38099. Title: A Prototype Problem-Solving Environment for Living With a Star Data Authors: Hurlburt, N.; Freeland, S.; Shine, R.; Bose, P. Bibcode: 2001AGUFMSH31A0702H Altcode: The Living With a Star program aims to understanding our space environment as a unified system. For this approach to be successful, the scientific working environment must present the LWS components as a unified whole. We present an architecture and data assimilation environment which addresses this critical issue. The goal of our Problem-Solving Environment for Living With a Star (PSELWS) project is to place the users of the data at center stage -- providing a virtual workbench with the tools, and infrastructure needed for seamless, timely and efficient access to the various data sources. Title: More Rotating Sunspot Observations by TRACE With Twisting EUV Coronal Fans Authors: Nightingale, R. W.; Shine, R. A.; Brown, D. S.; Wolfson, C. J.; Frank, Z. A.; Title, A. M. Bibcode: 2001AGUSM..SH41B11N Altcode: In an on-going search several sunspots, rotating about their umbral centers, have been identified in TRACE photospheric white light (WL) images. In many cases the rotation can also be seen in the corresponding UV (1600 Å) and/or EUV (171, 195 Å) images. Preliminary analysis of one such rotating sunspot and the coronal response to the rotation, observed in AR9114 on August 8-10, 2000, was presented at the fall AGU meeting (Nightingale et al., Abstract SH11A-10, EOS, AGU 2000 Fall Meeting, Vol. 81, p. F977, Nov. 2000). Further detailed analysis and modeling of this event, where loops appear to cross over one another, is in progress. Meanwhile, we are finding other examples within the TRACE data set. Twisting EUV coronal fans have been observed above rotating sunspots on August 16, 1999 for AR8667, where a sigmoid was visible in Yohkoh SXT data, and on May 20, 2000. Several rotating sunspots were also seen in the active region of the July 14, 2000 Bastille Day event. More recent rotations observed only in WL and UV occurred on December 11 and 22, 2000. Movies of some of these rotations will be shown, as well as magnetic field data from MDI on SOHO where available. Analysis of the rotational rates of the sunspots will be given. These observations display the coupling of the magnetic field from the photosphere into the corona. This work was supported by NASA under contract NAS5-38099. Title: Formation of Compact Coronal Structures Associated with the Emerging Magnetic Flux Authors: Ryutova, M. P.; Shine, R.; Tarbell, T. D. Bibcode: 2001AGUSM..SH32C01R Altcode: We study the events associated with the emergence of magnetic flux in the photosphere occurring throughout the solar atmosphere from its surface up to the low corona using coordinated observations from Swedish Vacuum Solar Telescope (SVST) on La Palma, the TRACE satellite and the MDI instrument on SOHO. The object of the observations is a plage dominated initially (UT 08:01:03, June 10, 1999) by positive polarity elements with about 0.3 magnetic filling factor near the same polarity sunspot. High resolution MDI magnetograms are assembled in a 6-hour movie and co-aligned with TRACE Fe IX/X 171 Å images of the corona, SVST Ca II K-line images showing the low chromosphere and Hα filtergrams showing plasma motions higher in the chromosphere. To study line of sight motions, we used filtergrams taken in the +/- 350 ~mÅ (and +/- 700 ~mÅ) wings of Hα . During the first two hours, there are almost no changes (at the MDI resolution) in the initial magnetic field pattern of studied region, and the 171 Å emission above this region shows stable amorphous structures. Then a series of events lead to the formation of two opposite polarity pores in the target region and compact coronal loops above it with the following chronology. First, opposite polarity small-scale flux tubes emerge and interact with the existing plage elements. This is followed almost immediately by strong Hα surges, whose peak activity lasts about 10 minutes. After this lag, enhanced emission in 171 Å takes the form of a short-lived transient. During the next one hour (long before the pore and compact coronal loops form), there are several new Hα surges and coronal plasma jets whose activity correlates well with remarkable changes in the photospheric fluxes which eventually form pores. For a quantitative analysis we apply a theoretical model of energy transport from subsurface motions associated with the emerging magnetic flux. Strong disturbances generated in a limited surface area may propagate upward like blast waves along a cone. This in turn may cause a sequence of phenomena associated with forward and reflected shocks, whose signatures are similar to the observations. The process may last as long as significant changes in the photospheric magnetic field occur, until it is suppressed by the strong fields in the pores. Under some condition the established pore structure may be accompanied by a current drive which leads to formation of the coronal loops. Title: Sunspots: Moving Magnetic Features and Moat Flow Authors: Shine, R.; Title, A. Bibcode: 2000eaa..bookE2038S Altcode: Most mature SUNSPOTS and some large SUNSPOT PORES are surrounded, at least in part, by a zone which is free of stationary magnetic field (e.g. PLAGE, network) and which exhibits a radially outward horizontal mass flow. This zone is called a sunspot `moat'. The most notable features in the moat are small magnetic structures of mixed polarity called moving magnetic features (MMFs). These are trans... Title: Sunspot Oscillations from the Photosphere to the Corona Authors: Shine, R. A. Bibcode: 2000SPD....31.0303S Altcode: 2000BAAS...32Q.834S Denied the radiative splendor of the rest of the solar surface, sunspots seem to be compensated with more vigorous oscillations above their dark interiors. The observational properties of these oscillations will be reviewed along with some possibilities for employing them to study sunspot structure. The most obvious of these phenomena are the umbral oscillations and penumbral running waves seen in the chromosphere. Discovered in the late 1960's, umbral oscillations exhibit well documented non-linear behavior leading to shocks and umbral flashes in the upper chromosphere and transition region. Periods are typically 150 - 180s and are thought to be driven by photospheric motions. Running penumbral waves, best seen in H alpha or Na I D Dopplergrams, have periods near 250s and move outward in the penumbra with horizontal velocities from 10 - 25 km/s. Observations with the SMM/UVSP instrument showed that sunspot oscillations extended into the transition region and recent results from the CDS and SUMER instruments on SOHO show this in much more detail. The TRACE satellite has shown that coronal EUV loops (Fe IX 171 Angstroms and Fe X 195 Angstroms) originating in sunspots exhibit prominent intensity oscillations wherever they overlay the photospheric penumbra or umbra. Loops not associated with sunspots occasionally show similar oscillations but most do not. Some recent coordinated TRACE and H alpha observations (from the SVST on La Palma) will be presented to establish the relationships between the chromospheric and coronal oscillations. This work is supported by the TRACE and SOI/MDI projects at LMSAL and Stanford (contract NAS5-38099 and grant NAG5-3077). Title: TRACE Observations of Active Region Births Authors: Wolfson, C. J.; Shine, R. A. Bibcode: 2000SPD....31.0142W Altcode: 2000BAAS...32..808W TRACE has recorded the births of a few bona-fide active regions, as well as many ephemeral regions and so-called X-ray bright points. The observations have usually been made serendipitously while studying a nearby, well formed active region. However, a couple of events have been recorded when deliberately looking for emerging flux in quiet portions of an active region belt. This poster will discuss some of the best observations to date, where the quality ranking of the observation is closely coupled to the observing mode TRACE was in and the availability of high resolution (temporal and/or spatial) MDI magnetograms. Included will be the birth of NOAA AR#8699 on 11 September 1999 at about 14 UT (N22E34), AR#8637 on 17 July 1999 at about 4 UT (N11W1), and AR#8885 on 21 February 2000 at about 6 UT (N11W7); these specifics being provided to encourage coordination with other observations. The temporal relationships between the first appearances of magnetic bipoles, EUV loops, chromospheric plage, pores, and sunspots will be discussed as will the growth rate and spatial relationships of these different features and any associated photospheric flows. Title: Coordinated MDI/TRACE/SVST Observations of Sunspots Authors: Bush, R. I.; Shine, R. A.; Brandt, P.; Sobotka, M.; Scharmer, G. Bibcode: 2000SPD....31.0122B Altcode: 2000BAAS...32R.804B During the first two weeks of June 1999, coordinated observations of sunspots were made by the MDI instrument on the SOHO spacecraft, the TRACE satellite and the Swedish Vacuum Solar Tower (SVST) at La Palma. The MDI instrument was operating in a "high resolution" mode and was obtaining 1.2 arc-second resolution magnetograms and 2.4 arc-second resolution dopplergrams at a one minute cadence. TRACE observations were made in Fe IX/X 171 Angstroms and/or Fe XII 195 Angstroms together with the 1600 Angstroms and continuum bands at a 1.0 arc-second resolution. The SVST data consist of filtergrams taken with three 2Kx2K CCD cameras with about 0.4 arc-second resolution operating in frame selection mode. The first camera used a fixed G band (4305 Angstroms) filter, the second a fixed blue continuum filter (4507 Angstroms), and the third a narrow band tunable filter which was cycled through several positions in the Hα line and the 6302 Angstroms Fe ~I line. The goal of this investigation is to detail the evolution of stable sunspots in order to understand the detailed correlation of photospheric flows and magnetic features. The high time and spatial resolution of these measurements provides a unique opportunity to explore the interactions of plasma and magnetic field at the solar surface. This work was supported by NASA grant NAG5-3077 at Stanford and NASA contract NAS5-38099 at Lockheed Martin. Title: Electro-Mechanical Coupling Between the Photosphere and Transition Region Authors: Tarbell, T. D.; Ryutova, M.; Shine, R. Bibcode: 2000SoPh..193..195T Altcode: We study the response of the chromosphere and transition region to dynamic changes in the photospheric network magnetic fields. We present results from simultaneous measurements taken by TRACE in chromospheric and transition region (C iv) images, high-resolution magnetograms taken by MDI, and spectra of chromospheric (C ii) and transition region lines (O vi) obtained with the SUMER instrument on SOHO. Enhanced emission in the C iv line is generally co-spatial with the magnetic pattern in the photosphere. We propose a mechanism of electro-mechanical coupling between the photosphere and upper layers of atmosphere based on hydrodynamic cumulation of energy produced by reconnecting flux tubes in the photosphere/chromosphere region (Tarbell et al., 1999). We believe that a basic process causing energetic events is the cascade of shock waves produced by colliding and reconnecting flux tubes. The continuous supply of flux tubes in the `magnetic carpet' ensures the ubiquitous nature of this process and its imprint on the upper atmosphere. The appearance of bright transients often, but not always, correlates with canceling mixed polarity magnetic elements in the photosphere. In other cases, transients occur in regions of unipolar flux tubes, suggesting reconnection of oblique components. Transients are also seen in regions with no fields detected with the MDI sensitivity; these may be reconnections of tiny features with diameters less than 100 km. Blinkers and other bright transients are often accompanied by two directional plasma jets. These may be generated by cylindrical self-focusing of shock fronts or by collision of shocks produced by neighboring reconnection processes. The observations suggest that stronger emissions correspond to lower velocity jets, and vice versa; this property is a natural consequence of the proposed mechanism. Plasma flows are always seen whenever the slit crosses strong magnetic flux tubes or vertices of converging flows in the supergranular network. The overall energy distribution between heating and plasma flows is an intrinsic feature of our mechanism. Title: Supergranule and Mesogranule Evolution Authors: Shine, R. A.; Simon, G. W.; Hurlburt, N. E. Bibcode: 2000SoPh..193..313S Altcode: The MDI instrument on the SOHO satellite obtained a nearly continuous 45.5-hr run in high-resolution mode on 17-18 January 1997, collecting continuum, Dopplergram, and magnetogram images once per minute. This is one of the longest data sets yet obtained in this mode and shows significant evolution of the supergranulation pattern. After allowing for solar rotation within the fixed field of view, an area spanning 17° in latitude and 11° in longitude was extracted that covers the same area of the solar surface for the entire run. From the de-rotated continuum images, we computed flow maps of photospheric motions using local correlation techniques (LCT). Horizontal divergence maps constructed from the flow maps show local maxima of the size of mesogranules (5-10''). We interpret these as mesogranules although the LCT flow map resolution (4.8'' FWHM) may not completely resolve smaller mesogranules. Movies made from the divergence maps clearly show the outward convection (advection) of these mesogranules within each supergranule, and narrow boundaries of negative divergence outlining the supergranules. Several new supergranules are observed forming. These appear as areas of strong divergence that pop up between pre-existing supergranules and grow, pushing their neighbors apart. Others seem to perish between growing neighbors. We also computed the vertical component of vorticity from the flow maps. Movies of this vorticity do not show any obvious patterns. Title: Bright Chromospheric Grains and the Magnetic Intranetwork Authors: Worden, John; Harvey, John; Shine, Richard Bibcode: 1999ApJ...523..450W Altcode: We compare bright grains in the cell interiors of the chromospheric network with intranetwork magnetic field elements using images from the Transition Region and Coronal Explorer Satellite (TRACE) taken at H I Lyα (121.6 nm) (chromosphere) and the continuum at 160 nm (temperature minimum).We find only a random correspondence between bright cell grains and regions of intranetwork magnetic flux as seen in these two emissions. In addition, we find that the 160.0 nm cell grains that do overlay magnetic intranetwork show no correlation between intensity and magnetic field strength. However, it is possible that Lyα bright cell grains that overlay magnetic fields may show a slight enhancement in intensity. Our results suggest that the intranetwork magnetic field is essentially uninvolved with the production of cell grains in the upper photosphere/lower chromosphere but could have a small involvement with bright cell grains in the chromosphere/transition region. Title: A new view of the solar outer atmosphere by the Transition Region and Coronal Explorer Authors: Schrijver, C. J.; Title, A. M.; Berger, T. E.; Fletcher, L.; Hurlburt, N. E.; Nightingale, R. W.; Shine, R. A.; Tarbell, T. D.; Wolfson, J.; Golub, L.; Bookbinder, J. A.; DeLuca, E. E.; McMullen, R. A.; Warren, H. P.; Kankelborg, C. C.; Handy, B. N.; De Pontieu, B. Bibcode: 1999SoPh..187..261S Altcode: The Transition Region and Coronal Explorer (TRACE) - described in the companion paper by Handy et al. (1999) - provides an unprecedented view of the solar outer atmosphere. In this overview, we discuss the initial impressions gained from, and interpretations of, the first million images taken with TRACE. We address, among other topics, the fine structure of the corona, the larger-scale thermal trends, the evolution of the corona over quiet and active regions, the high incidence of chromospheric material dynamically embedded in the coronal environment, the dynamics and structure of the conductively dominated transition region between chromosphere and corona, loop oscillations and flows, and sunspot coronal loops. With TRACE we observe a corona that is extremely dynamic and full of flows and wave phenomena, in which loops evolve rapidly in temperature, with associated changes in density. This dynamic nature points to a high degree of spatio-temporal variability even under conditions that traditionally have been referred to as quiescent. This variability requires that coronal heating can turn on and off on a time scale of minutes or less along field-line bundles with cross sections at or below the instrumental resolution of 700 km. Loops seen at 171 Å (∼1 MK) appear to meander through the coronal volume, but it is unclear whether this is caused by the evolution of the field or by the weaving of the heating through the coronal volume, shifting around for periods of up to a few tens of minutes and lighting up subsequent field lines. We discuss evidence that the heating occurs predominantly within the first 10 to 20 Mm from the loop footpoints. This causes the inner parts of active-region coronae to have a higher average temperature than the outer domains. Title: The transition region and coronal explorer Authors: Handy, B. N.; Acton, L. W.; Kankelborg, C. C.; Wolfson, C. J.; Akin, D. J.; Bruner, M. E.; Caravalho, R.; Catura, R. C.; Chevalier, R.; Duncan, D. W.; Edwards, C. G.; Feinstein, C. N.; Freeland, S. L.; Friedlaender, F. M.; Hoffmann, C. H.; Hurlburt, N. E.; Jurcevich, B. K.; Katz, N. L.; Kelly, G. A.; Lemen, J. R.; Levay, M.; Lindgren, R. W.; Mathur, D. P.; Meyer, S. B.; Morrison, S. J.; Morrison, M. D.; Nightingale, R. W.; Pope, T. P.; Rehse, R. A.; Schrijver, C. J.; Shine, R. A.; Shing, L.; Strong, K. T.; Tarbell, T. D.; Title, A. M.; Torgerson, D. D.; Golub, L.; Bookbinder, J. A.; Caldwell, D.; Cheimets, P. N.; Davis, W. N.; Deluca, E. E.; McMullen, R. A.; Warren, H. P.; Amato, D.; Fisher, R.; Maldonado, H.; Parkinson, C. Bibcode: 1999SoPh..187..229H Altcode: The Transition Region and Coronal Explorer (TRACE) satellite, launched 2 April 1998, is a NASA Small Explorer (SMEX) that images the solar photosphere, transition region and corona with unprecedented spatial resolution and temporal continuity. To provide continuous coverage of solar phenomena, TRACE is located in a sun-synchronous polar orbit. The ∼700 Mbytes of data which are collected daily are made available for unrestricted use within a few days of observation. The instrument features a 30-cm Cassegrain telescope with a field of view of 8.5×.5 arc min and a spatial resolution of 1 arc sec (0.5 arc sec pixels). TRACE contains multilayer optics and a lumogen-coated CCD detector to record three EUV wavelengths and several UV wavelengths. It observes plasmas at selected temperatures from 6000 K to 10 MK with a typical temporal resolution of less than 1 min. Title: A new view of the solar corona from the transition region and coronal explorer (TRACE) Authors: Golub, L.; Bookbinder, J.; Deluca, E.; Karovska, M.; Warren, H.; Schrijver, C. J.; Shine, R.; Tarbell, T.; Title, A.; Wolfson, J.; Handy, B.; Kankelborg, C. Bibcode: 1999PhPl....6.2205G Altcode: The TRACE Observatory is the first solar-observing satellite in the National Aeronautics and Space Administration's (NASA) Small Explorer series. Launched April 2, 1998, it is providing views of the solar transition region and low corona with unprecedented spatial and temporal resolution. The corona is now seen to be highly filamented, and filled with flows and other dynamic processes. Structure is seen down to the resolution limit of the instrument, while variability and motions are observed at all spatial locations in the solar atmosphere, and on very short time scales. Flares and shock waves are observed, and the formation of long-lived coronal structures, with consequent implications for coronal heating models, has been seen. This overview describes the instrument and presents some preliminary results from the first six months of operation. Title: Observations of Filaments Authors: Title, A.; Schrijver, C.; Tarbell, T.; Shine, R. Bibcode: 1999AAS...194.7905T Altcode: 1999BAAS...31..963T Filaments are clearly seen as absorption features in the TRACE FE IX and XII images. Because of the 24 hour coverage of TRACE many filaments have been observed on the disk and near the limb, and as quiescent and active structures. A quiescent filament consists of many parallel strands the run nearly parallel to the surface. The strands are often at the TRACE resolution and are always in motion. Adjacent strands often exhibit flows in opposite directions with speeds of 10 to 40 km/second. Filaments occasionally erupt explosive from the surface. The initial accelerations have not been observed with a 30 second cadence. Velocities in the initial phase range between 200 and 400 km/s. Filaments are observed to erupt and travel out of the TRACE field of view, erupt and fall back to the solar surface, and erupt and travel a short distance before being constraint by overlying fields. Examples of the dynamic structure of filaments and their modes of eruption will be demonstrated in a video presentation. Title: Dispersal of Magnetic Flux in the Quiet Solar Photosphere Authors: Hagenaar, H. J.; Schrijver, C. J.; Title, A. M.; Shine, R. A. Bibcode: 1999ApJ...511..932H Altcode: We study the random walk of magnetic flux concentrations on two sequences of high-resolution magnetograms, observed with the Michelson Doppler Imager on board SOHO. The flux contained in the concentrations ranges from |Φ|=1018 Mx to |Φ|=1019 Mx, with an average of |Φ|=2.5×1018 Mx. Larger concentrations tend to move slower and live longer than smaller ones. On short timescales, the observed mean-square displacements are consistent with a random walk, characterized by a diffusion coefficient D(t<10 ks)=70-90 km2 s-1. On longer timescales, the diffusion coefficient increases to D(t>30 ks)=200-250 km2 s-1, approaching the measurements for a five-day set of Big Bear magnetograms, D~=250 km2 s-1. The transition between the low and large diffusion coefficients is explained with a model and simulations of the motions of test particles, subject to random displacements on both the granular and supergranular scales, simultaneously. In this model, the supergranular flow acts as a negligible drift on short timescale, but dominates the granular diffusion on longer timescales. We also investigate the possibility that concentrations are temporarily confined, as if they were caught in supergranular vertices, that form short-lived, relatively stable environments. The best agreement of model and data is found for step lengths of 0.5 and 8.5 Mm, associated evolution times of 14 minutes and 24 hr, and a confinement time of no more than a few hours. On our longest timescale, DSim(t>105)-->285 km2 s-1, which is the sum of the small- and large-scale diffusion coefficients. Models of random walk diffusion on the solar surface require a larger value: DWang=600+/-200 km2 s-1. One possible explanation for the difference is a bias in our measurements to the longest lived, and therefore slower concentrations in our data sets. Another possibility is the presence of an additional, much larger diffusive scale. Title: Dynamics of the Quiet Solar Chromosphere Authors: Rutten, R. J.; Lites, B. W.; Berger, T. E.; Shine, R. A. Bibcode: 1999ASPC..158..249R Altcode: 1999ssa..conf..249R No abstract at ADS Title: Supergranule and Mesogranule Evolution Authors: Shine, Richard; Simon, George; Hurlburt, Neal Bibcode: 1999soho....9E..15S Altcode: The MDI instrument on the SoHO satellite obtained a nearly continuous 46-hour run in high resolution mode on January 17 to 18, 1997, collecting continuum, dopplergram, and magnetogram images once per minute. This is one of the longest data sets yet obtained in this mode and shows significant evolution of the supergranulation pattern. After allowing for solar rotation within the fixed field of view, an area spanning 13 degrees in latitude and 10 degrees in longitude was extracted that covers the same area of the solar surface for the 46 hours. Using the derotated continuum images, we computed flow maps of photospheric motions using local correlation techniques (LCT). The accuracy of these LCT's has been verified by comparison with La Palma ground based data using other data sets (Shine, et al, 1997, B.A.A.S., 29, 02.62). Horizontal divergence maps constructed from the flow maps show local maxima of about the size of mesogranules. We interpret these as mesogranules although the LCT flow map resolution (4.8 arc seconds FWHM) may not completely resolve all mesogranules. Movies made from the divergence maps clearly show the outward convection of these "mesogranules" within each supergranule and narrow boundaries of negative divergence outlining the supergranules. Several new supergranules are observed forming as areas of strong divergence that pop up between pre-existing supergranules and grow, pushing their neighbors apart. Others seem to perish between growing neighbors. Movies of the derived vertical curl do not show any obvious patterns. Videos of these movies and the continuum, dopplergram, and magnetogram images will be shown. This work was supported by NASA Grant NAG5-3077 at Stanford and Lockheed Martin. Title: Measurements of Solar Magnetic Element Dispersal Authors: Berger, Thomas E.; Löfdahl, Mats G.; Shine, Richard A.; Title, Alan M. Bibcode: 1998ApJ...506..439B Altcode: The dispersal of magnetic elements in the solar photospheric flow field is studied by tracking individual ``magnetic bright points'' (MBPs) identified in a G-band 4305 Å filtergram time series obtained at the 50 cm Swedish Vacuum Solar Telescope on La Palma, Spain. The time series spans approximately 70 minutes with a field of view of 29" × 29" near disk center. All images in the time series are restored to near the telescope diffraction limit (~0.2" in the G band) using partitioned phase diverse speckle techniques. Regions of enhanced magnetic network and quiet Sun are examined. In the network region, automated tracking of individual MBPs reveals approximately Gaussian diffusion, with indications for slightly ``superdiffusive'' dispersal. The inferred Gaussian diffusion coefficient is 60.4 +/- 10.9 km2 s-1. In the quiet-Sun region, local correlation tracking velocity measurements show the dispersal of artificial tracers to be non-Gaussian over most of our data set with indications of an asymptotic approach to a 285 km2 s-1 Gaussian diffusion. Title: Large-scale coronal heating by the small-scale magnetic field of the Sun Authors: Schrijver, C. J.; Title, A. M.; Harvey, K. L.; Sheeley, N. R.; Wang, Y. -M.; van den Oord, G. H. J.; Shine, R. A.; Tarbell, T. D.; Hurlburt, N. E. Bibcode: 1998Natur.394..152S Altcode: Magnetic fields play a crucial role in heating the outer atmospheres of the Sun and Sun-like stars, but the mechanisms by which magnetic energy in the photosphere is converted to thermal energy in the corona remain unclear. Observations show that magnetic fields emerge onto the solar surface as bipolar regions with a broad range of length scales. On large scales, the bipolar regions survive for months before dispersing diffusively. On the smaller scales, individual bipolar regions disappear within days but are continuously replenished by new small flux concentrations, resulting in a sustained state of mixed polarity. Here we determine the rate of emergence of these small bipolar regions and we argue that the frequent magnetic reconnections associated with these regions (an unavoidable consequence of continued flux replacement) will heat the solar atmosphere. The model that describes the details of these mixed-polarity regions is complementary to the traditional diffusion model for large-scale flux dispersal and a combination of the two should lead to a more complete understanding of the role of magnetic fields in stellar atmospheres. Title: First Results from the TRACE Mission Authors: Title, A.; Tarbell, T.; Schrijver, C.; Wolfson, J.; Shine, R.; Hurlburt, N.; Golub, L.; Deluca, E.; Bookbinder, J.; Handy, B.; Acton, L.; Harrison, R.; Delaboudinere, J. -P. Bibcode: 1998AAS...192.1507T Altcode: 1998BAAS...30..841T The TRACE spacecraft was launched on 1 April and all systems are functioning as designed. The initial outgassing period will conclude on 20 April and the science program will then begin. TRACE is a UV-EUV imager with one arc second spatial resolution and is capable of taking images with a cadence as high as two seconds. We will present images and image sequences. We hope to present initial comparisons of magnetic evolution and transition region and coronal brightenings. Title: The Postflare Loops and the Nearby Active Chromosphere of 1992 June 26: Addendum Authors: Malherbe, J. -M.; Tarbell, T.; Wiik, J. E.; Schmieder, B.; Frank, Z.; Shine, R. A.; van Driel-Gesztelyi, L. Bibcode: 1998ApJ...495..502M Altcode: Video segments are presented that were processed from a quantitative study of the dynamics of the evolution of Hα postflare loops developed after a large solar flare. The high spatial resolution of the Swedish Vacuum Solar Telescope (SVST) at La Palma provided a unique set of data for such an event. Title: Small-scale topology of solar atmosphere dynamics. I. Wave sources and wave diffraction Authors: Hoekzema, N. M.; Rutten, R. J.; Brandt, P. N.; Shine, R. A. Bibcode: 1998A&A...329..276H Altcode: We study the small-scale topology of dynamical phenomena in the quiet-sun internetwork atmosphere, using short-duration Fourier analysis of high-resolution filtergram sequences to obtain statistical estimates for the co-location probability of different fine-structure elements and wave modes. In this initial paper we concentrate on the topology of short-duration Fourier amplitude maps for the photosphere and the simultaneously observed overlying chromosphere. We find that these maps portray a complex mix of global modes and locally excited waves which necessitates a statistical approach. Various aspects including mesoscale patterning indicate the presence of subsurface wave sources and of subsurface wave diffraction by convective inhomogeneities. Title: A Possible Mechanism for the Origin of Emerging Flux in the Sunspot Moat Authors: Ryutova, M.; Shine, R.; Title, A.; Sakai, J. I. Bibcode: 1998ApJ...492..402R Altcode: Mass and energy flow near sunspots are associated with the emergence of magnetic flux, which then moves outward in the sunspot moat. We present results of analytical and numerical studies of the interaction of horizontal magnetic flux and plasma flows in three-dimensional geometry. We show that nonlinear coupling of flux and plasma flows in the presence of a gravitational field lead to nonlinear dissipative instabilities that result in the formation of a solitary kink along the magnetic flux. The stability of a kink and its further evolution depend on the physical parameters of magnetic flux and the surrounding medium. We discuss two major cases--magnetic soliton-like and shocklike propagation along the magnetic flux--and specify the appropriate physical conditions for their realization. In photospheric conditions, the proposed mechanism may be a good candidate for understanding of the dynamics of small-scale magnetic flux in the enhanced network at the solar surface.

We apply our results to the observed properties of emerging flux in the sunspot region associated with moving magnetic features and find reasonable qualitative and quantitative agreement. Title: Photospheric flows as measured by SOI/MDI Authors: Hurlburt, N.; Frank, Z.; Shine, R.; Tarbell, T.; Title, A.; Simon, G. Bibcode: 1997ASSL..225..285H Altcode: 1997scor.proc..285H On 2 February and 7 March 1996, MDI on the SOHO spacecraft ran several hours to provide high resolution continuum images to map the horizontal flows near the equator and pole by correlation tracking. Here we present preliminary results on the performance of the tracking technique in measuring the differential rotation profile. These preliminary results are compared with each other and with corresponding results of previous studies. Title: Modeling the distribution of magnetic fluxes in field concentrations in a solar active region Authors: Schrijver, Carolus J.; Title, Alan M.; Hagenaar, Hermance J.; Shine, Richard A. Bibcode: 1997SoPh..175..329S Altcode: Much of the magnetic field in solar and stellar photospheres is arranged into clusters of `flux tubes', i.e., clustered into compact areas in which the intrinsic field strength is approximately a kilogauss. The flux concentrations are constantly evolving as they merge with or annihilate against other concentrations, or fragment into smaller concentrations. These processes result in the formation of concentrations containing widely different fluxes. Schrijver et al. (1997, Paper I) developed a statistical model for this distribution of fluxes, and tested it on data for the quiet Sun. In this paper we apply that model to a magnetic plage with an average absolute flux density that is 25 times higher than that of the quiet network studied in Paper I. The model result matches the observed distribution for the plage region quite accurately. The model parameter that determines the functional form of the distribution is the ratio of the fragmentation and collision parameters. We conclude that this ratio is the same in the magnetic plage and in quiet network. We discuss the implications of this for (near-)surface convection, and the applicability of the model to stars other than the Sun and as input to the study of coronal heating. Title: Sustaining the Quiet Photospheric Network: The Balance of Flux Emergence, Fragmentation, Merging, and Cancellation Authors: Schrijver, Carolus J.; Title, Alan M.; van Ballegooijen, Adriaan A.; Hagenaar, Hermance J.; Shine, Richard A. Bibcode: 1997ApJ...487..424S Altcode: The magnetic field in the solar photosphere evolves as flux concentrations fragment in response to sheared flows, merge when they collide with others of equal polarity, or (partially) cancel against concentrations of opposite polarity. Newly emerging flux replaces the canceled flux. We present a quantitative statistical model that is consistent with the histogram of fluxes contained in concentrations of magnetic flux in the quiet network for fluxes exceeding ~2 × 1018 Mx, as well as with estimated collision frequencies and fragmentation rates. This model holds for any region with weak gradients in the magnetic flux density at scales of more than a few supergranules. We discuss the role of this dynamic flux balance (i) in the dispersal of flux in the photosphere, (ii) in sustaining the network-like pattern and mixed-polarity character of the network, (iii) in the formation of unipolar areas covering the polar caps, and (iv) on the potential formation of large numbers of very small concentrations by incomplete cancellation. Based on the model, we estimate that as much flux is cancelled as is present in quiet-network elements with fluxes exceeding ~2 × 1018 Mx in 1.5 to 3 days, which is compatible with earlier observational estimates. This timescale is close to the timescale for flux replacement by emergence in ephemeral regions, so that this appears to be the most important source of flux for the quiet-Sun network; based on the model, we cannot put significant constraints on the amount of flux that is injected on scales that are substantially smaller than that of the ephemeral regions. We establish that ephemeral regions originate in the convection zone and are not merely the result of the reemergence of previously cancelled network flux. We also point out that the quiet, mixed-polarity network is generated locally and that only any relatively small polarity excess is the result of flux dispersal from active regions. Title: The Postflare Loops and the Nearby Active Chromosphere of 1992 June 26 Authors: Malherbe, J. -M.; Tarbell, T.; Wiik, J. E.; Schmieder, B.; Frank, Z.; Shine, R. A.; van Driel-Gesztelyi, L. Bibcode: 1997ApJ...482..535M Altcode: The main objective of this paper is to present a quantitative study of the dynamics of the evolution of Hα postflare loops developed after a large solar flare and the processed videos produced from the observations. The high spatial resolution of the Swedish Vacuum Solar Telescope (SVST) at La Palma has provided a unique set of data for such an event. A Gaussian fitting method is proposed to derive intensities and Doppler shifts from observations taken at three wavelengths (Hα center and Hα +/- 0.07 nm). Moving condensations or ``blobs'' of cold material provide transverse velocities, which, together with the radial component, enable us to derive their velocity vector magnitude. Plasma velocities are around free-fall velocities near the top of the loops but are significantly smaller close to their footpoints, suggesting a deceleration mechanism. The loops are anchored in the chromosphere, which shows tremendous activity in the active region and in the nearby ``quiet Sun.'' Spicules and ejection of plasmoids are also observed at the limb. Title: On the Dynamics of Magnetic Flux Concentrations in Quiet Photospheric Network. Authors: Sakai, J. I.; Ryutova, M.; Schrijver, K.; Shine, R.; Tarbell, T.; Berger, T.; Title, A.; Hagenaar, H. Bibcode: 1997SPD....28.0260S Altcode: 1997BAAS...29..904S Magnetic flux concentrations in the quiet photospheric network show a complex dynamics which includes merging of colliding fluxes, the "total" or partial cancellation of neighboring fluxes, fragmentation and others. We propose a mechanism to explain the observed phenomena based on the idea that magnetic flux concentrations in the photospheric network are essentially non-collinear. We show that non-collinearity of colliding fluxes leads to the whole new class of effects which are observed; for example, the apparent cancellation of opposite polarity fluxes turns into the formation of horizontal magnetic fluxes (which later may appear as a new weaker bipoles) and is accompanied by the shock formation and mini-flares. In the case of shock formation the reconnection area becomes a source of the acoustic emission; mini-flares may be seen as bright points. The energetics of these processes strongly depends on geometry of "collision" and physical parameters of colliding fluxes. For example, if colliding fluxes have comparable and "small" cross sections, the reconnection results in complete reorganization of their magnetic fields; if merging fluxes are large enough or considerably different, magnetic flux may be only partially reconnected and partially survived. Reconnection of non-collinear equal polarity fluxes leads to the "scattering" processes which include the fragmentation into several smaller fluxes if initially colliding concentrations carried different amount of magnetic flux. We give the example of numerical simulation for the case of merging and fragmentation process occurring during the collision of collinear "strong" and "weak" magnetic flux concentrations. The calculation results shown to be consistent with observational data from both the SOHO/MDI instrument and the Swedish Vacuum Solar Telescope on La Palma. This research is supported by NASA contract NAG5-3077 at Stanford University and the MDI contract PR 9162 at Lockheed. Title: Nobeyama/SOHO/BBSO Comparison of Solar Polar Coronal Holes Authors: Gary, D. E.; Enome, S.; Shibasaki, K.; Gurman, J. B.; Shine, R. A. Bibcode: 1997SPD....28.0801G Altcode: 1997BAAS...29..912G Although it is not widely known outside the discipline of solar radiophysics, a long-standing puzzle exists: the poles of the Sun appear brighter than the rest of the quiet Sun in a restricted range of wavelengths roughly from 15 GHz to about 48 GHz (cf. Kosugi et al. 1986). At somewhat lower radio frequencies the poles appear darker than the quiet Sun due to a deficit of coronal material, while at mm-wavelengths the polar and non-polar quiet Sun appear quite uniform due to the similarity of the atmospheric structure at lower heights in the chromosphere. The excess brightness at the poles has also been reported in coronal holes on the disk, and so is apparently related to the phenomenon of coronal holes. The brightening likely corresponds to an elevated temperature in the upper chromosphere in coronal holes relative to normal quiet Sun. The phenomenon is especially well suited to study via radio emission due to the unique sensitivity of radio waves to this height range in the chromosphere. The possibility exists that the different chromospheric structure for coronal holes implied by the radio brightening may offer some clue to the origin of the fast solar wind, which is now well established to arise in coronal holes. Radio brightening of coronal holes is a difficult observational problem because an instrument is needed that can image large areas of the Sun at relatively high resolution. The Nobeyama Radioheliograph has the required capability and operates at 17 and 34 GHz, nicely within the frequency range where the brightening occurs. We compare Nobeyama radio synthesis images on several days in 1996 with images from the EIT, CDS, and MDI experiments on the Solar and Heliospheric Observatory (SOHO) spacecraft, and with high resolution images from the Big Bear Solar Observatory, with the aim of determining the spatial and temporal characteristics of the brightening. We compare the extent of the radio brightening with the boundaries of the coronal holes seen from the SOHO data, to establish the previously suggested identity of the polar brightening with coronal holes. We investigate whether the brightening is primarily associated with network features, faculae, or perhaps bipolar magnetic elements, or whether it is instead a diffuse brightening more-or-less uniformly covering the coronal hole area. We look for temporal variations, and their correlation with changing features seen from SOHO. We conclude with some ideas for how the chromospheric structure may be different in coronal holes than in normal quiet Sun, and speculate on the implications for acceleration of the fast solar wind. Title: Phase-Diversity Restoration of two Simultaneous 70-minute Photospheric Sequences. Authors: Lofdahl, M. G.; Berger, T. E.; Shine, R. A.; Title, A. M. Bibcode: 1997SPD....28.0218L Altcode: 1997BAAS...29..896L Seeing effects have been corrected in two cospatial and cotemporal 70-minute sequences of images collected in the G-band 4305 Angstroms and wideband 4686 Angstroms. The data were obtained with the 50 cm Swedish Vacuum Solar Telescope on the island of La Palma, Spain. The 29arcsecx 70arcsec field-of-view (FOV) near disk center contains both an enhanced network region and an (apparently) non-magnetic ``quiet'' region of granulation. The mean time between restored frames is 23.5 s. Each of the 180 images is created with Phase-Diverse Speckle (PDS) imaging, using two different focus positions sampled at the best three snapshots of the atmospheric turbulence (seeing) during a 20-second selection window. Wavefronts are estimated for each focused--defocused image pair and a restored frame is produced from all six images. The average resolution in the restored sequence is about 0farcs4 (corresponding to spatial frequencies up to half the diffraction limit of the telescope), which is good enough to allow detection of ~ 0farcs2 bright points. The data is used for statistical measurements of magnetic element speed, interaction frequency, and lifetime (see accompanying poster by T. E. Berger et al). We show destretched and space-time filtered movies of both the G-band and continuum images, as well as raw data to demonstrate the effect of the restoration process. This work was supported by NASA contracts NAS5-30386 at Stanford and NAS8-39747 and Independent Research Funds at Lockheed-Martin. MGL was supported by the Swedish Science Research Council. Title: Comparison of Granulation Correlation Tracking (CT) and Feature Tracking (FT) Results from SOHO/MDI and the Swedish Vacuum Solar Telescope on La Palma Authors: Shine, R.; Strous, L.; Simon, G.; Berger, T.; Hurlburt, N.; Tarbell, T.; Title, A.; Scharmer, G. Bibcode: 1997SPD....28.0262S Altcode: 1997BAAS...29Q.904S We have computed photospheric velocity flow maps from simultaneous observations taken with MDI and at the Swedish Vacuum Solar Tower (SVST) on La Palma on August 15, 1996. Both sets consist of a series of photospheric images, and flow maps are computed by following the local motions of granules. The MDI data have the important advantages of very stable images and longer continuous coverage of the same area of the solar surface. This longer coverage is necessary to study the evolution of mesogranules, supergranules, and to detect possible low amplitude motions on scales larger than supergranules. However, the high resolution mode of MDI is limited by the small telescope size to about 1.2 arc seconds angular resolution and uses a 0.6 arc second pixel size. This is adequate to show granulation but has the rms constrast significantly reduced to about 2%. Early efforts adapting techniques that were successful with higher resolution ground based images gave poor results and although new methods have now been developed, there are still some problems with accuracy. On the other hand, the SVST images have much higher angular resolution (as good as 0.2 arc second) but suffer from variable atmospheric distortion. They also have a much smaller field of view. By detailed comparison of the two data sets and by using CT and FT techniques to track the motions, we hope to understand the sources of any differences between them and to develop credible correction parameters to the MDI data sets if necessary. This work was supported by NASA Grant NAG5-3077 at Stanford and Lockheed Martin, by AFOSR and the Fellows Program of AF Phillips Lab at NSO/SP, and by the Swedish Royal Academy of Sciences. Title: Horizontal Velocity Structure of Supergranules near Disk Center from High-Resolution SoHO/MDI Observations Authors: Strous, L. H.; Simon, G. W.; Shine, R. A.; Hurlburt, N. Bibcode: 1997SPD....28.0265S Altcode: 1997BAAS...29S.904S We determine the average surface flows in supergranules from high-resolution SoHO/MDI observations near disk center, using local correlation and feature tracking methods. We present results as a function of distance to the supergranule center and of supergranule size, and as a function of normalized distance to the supergranule center. This work was supported by NASA Grant NAG5-3077 at Stanford and Lockheed Martin, and by AFOSR and the Fellows Program of AF Phillips Lab at NSO/SP. Title: A search for interaction between magnetic fields and supergranular flows in the network based on MDI observations Authors: Schrijver, C. J.; Shine, R. A.; Title, A. M.; Hagenaar, H. J.; Hurlburt, N. E.; Tarbell, T. D.; Simon, G. W. Bibcode: 1997SPD....28.0243S Altcode: 1997BAAS...29..901S We study the supergranular flow field and its temporal evolution in the quiet Sun as observed with the Michelson Doppler Imager on board SOHO. We use the intensity images to derive the flow fields using local correlation tracking. The data sets span one to two days with a one--minute cadence. We separate areas with a relatively high filling factor for magnetic concentrations from areas with a low magnetic filling factor in order to study to what extent the flows influence the magnetic network in the quiet Sun and vice versa. This work is supported by NASA Grant NAG5-3077 at Stanford and Lockheed Martin, and by AFOSR and the Fellows Program of AF Phillips Lab at NSO/SP Title: Continuous Observations of Solar Magnetic Fields from SOI/MDI on SOHO Authors: Hoeksema, J. T.; Bush, R. I.; Scherrer, P. H.; Heck, C.; Hurlburt, N.; Shine, R.; Tarbell, T.; Title, A. Bibcode: 1997SPD....28.0127H Altcode: 1997BAAS...29..884H The Solar Oscillations Investigation's Michelson Doppler Imager instrument (SOI/MDI) on SOHO measures the photospheric magnetic field over the whole disk nearly every 96 minutes with 4" resolution and a noise level of a few Gauss. Beginning in April 1996, this unprecedented continuous series of frequent, uniform quality magnetograms provides a striking view of the continual emergence, motion, evolution, and interaction of magnetic flux everywhere on the visible solar surface near solar minimum. These evolving photospheric fields ultimately drive the variations of the corona and solar wind that affect the terrestrial environment. Knowledge of the rapidly evolving photospheric field provides a crucial input for forecasting conditions in the corona, heliosphere, and geospace. A few magnetograms are available each day within hours of observation through the SOHO web site at http://sohowww.nascom.nasa.gov/. These may be used for planning and forecasting, e.g. to compute models of the solar corona. The remainder are generally available within a few weeks. Sometimes more focused campaigns provide magnetic observations as often as once each minute for up to 8 hours. Campaigns can be run with either the full disk resolution or with 0.6" pixels in a limited field near the center of the disk. The SOI project welcomes collaborations. More information can be found at http://soi.stanford.edu/. Title: Image Improvement Techniques Authors: Shine, R. A. Bibcode: 1997SPD....28.1202S Altcode: 1997BAAS...29..916S Over the last decade, a repertoire of techniques have been developed and/or refined to improve the quality of high spatial resolution solar movies taken from ground based observatories. These include real time image motion corrections, frame selection, phase diversity measurements of the wavefront, and extensive post processing to partially remove atmospheric distortion. Their practical application has been made possible by the increasing availability and decreasing cost of large CCD's with fast digital readouts and high speed computer workstations with large memories. Most successful have been broad band (0.3 to 10 nm) filtergram movies which can use exposure times of 10 to 30 ms, short enough to ``freeze'' atmospheric motions. Even so, only a handful of movies with excellent image quality for more than a hour have been obtained to date. Narrowband filtergrams (about 0.01 nm), such as those required for constructing magnetograms and Dopplergrams, have been more challenging although some single images approach the quality of the best continuum images. Some promising new techniques and instruments, together with persistence and good luck, should continue the progress made in the last several years. Title: Measurements of Magnetic Element Dynamics in the Network Authors: Berger, T. E.; Lofdahl, M. G.; Shine, R. A.; Title, A. M. Bibcode: 1997SPD....28.0219B Altcode: 1997BAAS...29..896B Statistical measurements of magnetic element speed, interaction frequency, and lifetime in an enhanced network region at disk center are presented. The primary dataset is a 70 min time series of G-band 4305 Angstroms filtergrams taken at the 50 cm Swedish Vacuum Solar Telescope (SVST) on the island of La Palma, Spain. A second time series of 4686 Angstroms wide-band continuum filtergrams, cospatial and simultaneous to within several milliseconds with the G-band images, is also studied. The field-of-view is near Sun center and includes a region of enhanced network activity with many G-band bright points. Both time series are corrected for seeing to very near the telescope diffraction limit by the technique of Phase Diverse Speckle (PDS) restoration (see accompanying poster by M. G. Lofdahl et al). We show destretched and space-time filtered movies of both the G-band and continuum images in two fields-of-view: a region of quiet granulation and the region of enhanced network activity. Within the network, local correlation tracking measurements on a 0\farcs4 grid show the RMS speed to be 778 m s(-1) ; outside the network the RMS speed is 1168 m s(-1) . Corkflow simulations show that normal convective flow patterns (granulation and mesogranulation) are absent in the network. Magnetic elements move with modal and mean speeds of 100 m s(-1) and 815 m s(-1) , respectively. The mean interaction frequency (time between either merging or splitting) is 220 s. The mean lifetime of tracked magnetic elements in the network is 9.33 min although 5% of the elements are tracked for the entire 70 min of the times series. This work was supported by NASA contracts NAS5-30386 at Stanford and NAS8-39747 and Independent Research Funds at Lockheed-Martin. MGL was supported by the Swedish Science Research Council. Title: Dispersal of magnetic flux in the quiet network as observed on a day-long magnetogram sequences observed with MDI on SOHO Authors: Hagenaar, H. J.; Schrijver, C. J.; Shine, R. A.; Title, A. M. Bibcode: 1997SPD....28.0244H Altcode: 1997BAAS...29..901H We study the dynamic behavior of magnetic flux elements in the quiet solar network using high--resolution magnetograms observed with the Michelson Doppler Imager on board SOHO. We track concentrations of magnetic flux in uninterrupted time sequences spanning 20 to 45 hours in order to study the dispersal of magnetic elements in the turbulent photospheric flows. We measure the displacements and derive average speeds as a function of time. The displacements are compared to a random walk model. This work is supported by NASA Grant NAG5-3077 at Stanford and Lockheed. Title: The TRACE Mission Authors: Wolfson, J.; Bruner, M.; Jurcevich, B.; Lemen, J.; Schrijver, K.; Shine, R.; Strong, K.; Tarbell, T.; Title, A.; Golub, L.; Bookbinder, J.; Deluca, E.; Acton, L.; Handy, B.; Kankelborg, C.; Fisher, R. Bibcode: 1997SPD....28.0143W Altcode: 1997BAAS...29..887W The TRACE (Transition Region and Coronal Explorer) mission will explore the connections between fine-scale magnetic fields and plasma structures in the coronal, transition zone and temperature minimum regions of the sun. TRACE will collect images of solar plasmas at temperatures from 10(4) to 10(7) K, with one arc second spatial resolution and excellent temporal resolution and continuity. With a scheduled launch date of 15 December 1997, the mission will emphasize collaborative observations with SoHO, enabling simultaneous observations of high-resolution images, spectra, and magnetograms. The 30 cm aperture TRACE telescope uses four normal-incidence coatings for the EUV and UV on quadrants of the primary and secondary mirrors. Interference filters further isolate 5 different UV bands. The images are co-aligned and internally stabilized against spacecraft jitter. A 1024 x 1024 lumigen-coated CCD detector collects images over an 8.5 x 8.5 arc minute field-of-view. LMATC, SAO, and GSFC built the TRACE instrument, which was integrated with the GSFC-produced SMEX spacecraft on 28 February (just over two years from the start of its development). It will be put into a Sun-synchronous orbit and operated in coordination with the SoHO Experiment Operations Facility at GSFC. We are committed to maintaining a publicly accessible data base for TRACE data. Browsing and data set requesting capabilities will be provided at Web site www.space.lockheed.com/TRACE/TRACElinks.html. This site already contains a large volume of information on the mission including preliminary scientific observing programs and directions as to how to participate in the mission now and in the future. This project is supported by NASA contract NAS5-38099. Title: Comparison of supergranular flows from doppler and local correlation tracking velocities Authors: Frank, Z.; Hurlburt, N.; Shine, R.; Tarbell, T.; Simon, G.; Strous, L.; Matt, S. Bibcode: 1997SPD....28.0259F Altcode: 1997BAAS...29..903F Measurements of the flows in the solar photosphere rely upon two techniques: doppler measurements of the line-of-sight velocity or tracking of features or patterns moving perpendicular to the line-of-sight. These methods have differing characteristics. Doppler measurements can easily measure surface flows near the limb which are not seriously contaminated by p-modes or other solar sources. However, they require excellent instrument calibration over the full field of view. Even then vertical flows within supergranules are barely detectable. Correlation and feature tracking have proven useful for estimating transverse velocity using granules and other tracers. Nevertheless, they can be degraded by the intensity variations of p-modes and possibly other oscillatory motions, as well as by effects of limb darkening and foreshortening. The two methods would both be strengthened through detailed comparisons. Data collected by MDI/SOHO is ideal for this purpose. The data is co-spatial and co-temporal, and is all obtained through the same instrument. We compare Doppler velocities with those obtained through correlation tracking using high-resolution MDI/SOHO images. We focus on motions at positions exceeding 30 degrees from disk center. After taking projection effects into account, we combine the two measurements to form a three-dimensional picture of the flows in the average supergranule. This work was supported by NASA Grant NAG5-3077 at Stanford and Lockheed Martin, and by AFOSR and the Fellows Program of AF Phillips Lab at NSO/SP. Title: The dynamic nature of the supergranular network Authors: Title, A. M.; Schrijver, C. J.; van Ballegooijen, A. A.; Hagenaar, H. J.; Shine, R. A. Bibcode: 1997SPD....28.0242T Altcode: 1997BAAS...29..900T The magnetic field in the quiet solar photosphere evolves as flux concentrations fragment in response to sheared flows, merge when they collide with others of equal polarity, or (partially) cancel against concentrations of opposite polarity. Newly emerging flux, mostly in ephemeral regions, replaces the canceled flux in a matter of a few days. We present a quantitative statistical model to describe the resulting histogram of fluxes contained in concentrations of magnetic flux in the quiet network. We discuss this dynamic flux balance with respect to (i) the potential dispersal of flux in the photosphere as a function of ephemeral-region properties, (ii) sustaining the network--like pattern and mixed--polarity character of the network, and (iii) the formation of unipolar areas covering the polar caps. We establish that ephemeral regions are not the result of the re-emergence of previously cancelled network flux. Moreover, their emergence cannot be correlated to the emergence of active regions but must instead be relatively homogeneous. We also point out that the bulk of the quiet, mixed-polarity network is generated locally, and that only any relatively small polarity excess is the result of flux dispersal from active regions. Title: Interactive interface for visualizing and analyzing multispectral solar images Authors: Hurlbert, Neal E.; Shine, Richard A.; Tarbell, Theodore D. Bibcode: 1997SPIE.3017..165H Altcode: We present an interactive software tool for manipulating image data, especially high resolution multi-spectral solar movies and images from several different instruments. This tool contains procedures for distortion removal for ground based solar movies, correlation tracking, image alignments, data compression, 3D FOurier filtering, interactive viewing of space/time slices in movies, and browsing through data cubes. This is a compete public domain package based on X windows and Unix which is currently running on Silicon Graphics and Digital Equipment workstations. These software tools are freely available to the international solar community. Many components are also applicable to image an movie analysis in astrophysics, space physics, and earth sciences. They are available with documentation via our web pages under http://www.space.lockheed.com. Title: On the dynamics of magnetic flux concentrations in quiet photospheric network. Authors: Sakai, J. I.; Ryutova, M.; Schrijver, K.; Shine, R. A.; Tarbell, T. D.; Berger, T. E.; Title, A. M.; Hagenaar, H. J. Bibcode: 1997BAAS...29T.904S Altcode: No abstract at ADS Title: The Dynamic Quiet Solar Corona: 4 Days of Joint Observing with MDI and EIT Authors: Schrijver, C. J.; Shine, R. A.; Hurlburt, N. E.; Tarbell, T. D.; Lemen, J. R. Bibcode: 1997ESASP.404..669S Altcode: 1997cswn.conf..669S No abstract at ADS Title: Dynamics of the Chromospheric Network: Mobility, Dispersal, and Diffusion Coefficients Authors: Schrijver, Carolus J.; Shine, Richard A.; Hagenaar, Hermance J.; Hurlburt, Neal E.; Title, Alan M.; Strous, Louis H.; Jefferies, Stuart M.; Jones, Andrew R.; Harvey, John W.; Duvall, Thomas L., Jr. Bibcode: 1996ApJ...468..921S Altcode: Understanding the physics behind the dispersal of photo spheric magnetic flux is crucial to studies of magnetoconvection, dynamos, and stellar atmospheric activity. The rate of flux dispersal is often quantified by a diffusion coefficient, D. Published values of D differ by more than a factor of 2, which is more than the uncertainties allow. We propose that the discrepancies between the published values for D are the result of a correlation between the mobility and flux content of concentrations of magnetic flux. This conclusion is based on measurements of displacement velocities of Ca II K mottles using an uninterrupted 2 day sequence of filtergrams obtained at the South Pole near cycle minimum. We transform the Ca II K intensity to an equivalent magnetic flux density through a power-law relationship defined by a comparison with a nearly simultaneously observed magnetogram. One result is that, wherever the network is clearly defined in the filtergrams, the displacement vectors of the mottles are preferentially aligned with the network, suggesting that network-aligned motions are more important to field dispersal than deformation of the network pattern by cell evolution. The rms value of the inferred velocities, R = <|v|2>½, decreases with increasing flux, Φ, contained in the mottles, from R ≍ 240 m s-1 down to 140 s-1. The value of R(Φ) appears to be independent of the flux surrounding the concentration, to the extreme that it does not matter whether the concentration is in a plage or in the network. The determination of a proper effective diffusion coefficient requires that the function R(Φ) be weighted by the number density n(Φ) of mottles that contain a total flux. We find that n(Φ) decreases exponentially with Φ and propose a model of continual random splitting and merging of concentrations of flux to explain this dependence. Traditional methods used to measure D tend to be biased toward the larger, more sluggish flux concentrations. Such methods neglect or underestimate the significant effects of the relatively large number of the more mobile, smaller concentrations. We argue that the effective diffusion coefficient for the dispersal of photo spheric magnetic flux is ∼600 km2 s-1. Title: A Possible Mechanism for the Origin Emerging Flux in the Sunspot Moat Authors: Sakai, Jun-Ichi; Shine, R.; Title, A.; Ryutova, M. Bibcode: 1996AAS...188.3502S Altcode: 1996BAAS...28R.871S Mass and energy flow near sunspots is associated with the emergence of magnetic flux which then moves outward in the sunspot moat. We present results of analytical and numerical studies of the interaction of horizontal magnetic flux and plasma flows in 3D-geometry. We show that nonlinear coupling of flux and plasma flows in the presence of a gravitational field lead to nonlinear dissipative instabilities which result in the formation of a solitary kink along the magnetic flux. The stability of a kink and its further evolution depends on the physical parameters of magnetic flux and surrounding medium. We discuss two major cases, magnetic soliton- and shock-like propagation along the magnetic flux, and specify the appropriate physical conditions for their realization. For example, under conditions in a sunspot moat, when the mass flow velocity exceeds about 0.5 v_A there occurs a magnetic soliton-like kink, propagating with a velocity less than the external mass flow velocity. The larger the radius of a flux tube, the larger the ``width'' of a soliton, and the lower the velocity of its propagation; the width of a soliton corresponds to the separation of ``legs'' of a kink which appear as magnetic field of the opposite polarities - the nearest to sunspot has obviously the same polarity. When the external mass flow velocity is less than about 0.5 v_A, a magnetic shock-like perturbation can propagate with a velocity larger than the external mass flow velocity. We apply these results to the observed properties of emerging flux and find reasonable qualitative and quantitative agreement. This research was supported by NASA contract NAG5-3077 at Stanford University (M.R.) and NASA contract NAS8-39747 at Title: Initial Results from SOI/MDI High Resolution Magnetograms Authors: Title, A.; Tarbell, T.; Frank, Z.; Schrijver, C.; Shine, R.; Wolfson, J.; Zayer, I.; Scherrer, P.; Bush, R.; Deforest, C.; Hoeksema, T. Bibcode: 1996AAS...188.6915T Altcode: 1996BAAS...28..938T The Michelson Doppler Imager (MDI) on SoHO takes magnetogram s with resolutions of 1.2 (high resolution) and 4 (full disk) arcseconds. Movies of 16 hour duration have been constructed in full disk and high resolution mode. High resolution movies of the south polar region also have been obtained. In sums of nine high resolution magnetograms it is possible to detect fields as low as 5 gauss and total fluxes as low as 5 10(1) 6 Mx. In mid latitude regions new flux is observed to emerge everywhere. At all latitudes below 60 degrees flux is mixed on the scale of supergranulation. In the polar region above 60 degrees only fields of a single polarity are observed above the detection limit. Title: Preliminary SOI/MDI Observations of Surface Flows by Correlation Tracking in the Quiet Solar Photosphere and an Emerging Active Region Authors: Tarbell, T.; Frank, Z.; Hurlburt, N.; Saba, J.; Schrijver, C.; Shine, R.; Title, A.; Simon, G.; Strous, L. Bibcode: 1996AAS...188.6914T Altcode: 1996BAAS...28..937T The extended observation of the solar surface with frequent sampling provided by MDI on SoHO offers the chance to observe the evolution of supergranules and to measure surface flows associated with active regions and perhaps larger scale zonal and meridonal flows. We have used local correlation tracking of the granulation pattern for measuring surface flows from MDI high resolution continuum images. The datasets consist of 1024 x 1024 pixel images collected with a cadence of one minute and extending many hours each. The images are typically centered upon the central meridian of the sun and offset to the north of sun center, spanning roughly 40 degrees of solar longitude and from approximately -10 to +30 degrees of solar latitude. The latitude dependence of the differential rotation is evident. We present preliminary results of our search for signatures of mesogranules, supergranules and giant cells. On 23 Feb. 1996, we obtained a 12-hour continuous sequence including quiet sun near disk center and NOAA region 7946 at about N08 E30. The active region grew rapidly over this interval, forming several sunpots. We show preliminary comparisons of the measured flow fields with coaligned SOI/MDI magnetograms taken at 15-minute intervals. The SOI/MDI program is supported by NASA grant NAG5-3077. Title: SOI/MDI Measurements of Horizontal Flows in the South Polar Region of the Sun by Correlation Tracking and Doppler Shifts Authors: Simon, G.; Frank, Z.; Hurlburt, N.; Schrijver, C.; Shine, R.; Tarbell, T.; Title, A.; Deforest, C. Bibcode: 1996AAS...188.6913S Altcode: 1996BAAS...28R.937S On 7 March 1996, the SOHO spacecraft was offset from its usual disk center pointing for an 11-hour observation of the South Polar region. MDI took a continuous time series of high resolution longitudinal magnetograms during this period, in support of the SOHO-wide Joint Observing Program on polar plumes. It also ran several hours each of two other programs: one to map the horizontal flows near the pole by correlation tracking and Doppler shifts, and another to study wave propagation (e.g., by time-distance helioseismology) at these high latitudes. In this poster we present preliminary results from the first program. Both techniques yield measurements of the differential rotation profile near the pole and of horizontal flows of supergranulation. These results are compared with each other and with corresponding measurements in low latitudes. The location of magnetic features in the horizontal flows is also shown. The SOI/MDI program is supported by NASA grant NAG5-3077. Title: Photospheric Surface Flows and Small Magnetic Structures in Sunspot Moats Authors: Shine, R. A.; Title, A.; Frank, Zoe; Scharmer, G. Bibcode: 1996AAS...188.3501S Altcode: 1996BAAS...28Q.871S We have computed horizontal flow maps of the photosphere around and within three different sunspots using high spatial resolution continuum movies obtained at the Swedish Vacuum Solar Telescope on La Palma on June 5, 1993, August 29, 1993, and July 14, 1994. Two of the data sets also included magnetograms and dopplergrams. A new feature found in the flow maps is azimuthal structure in the moat flows surrounding sunspots. Instead of a simple radial flow, there are zones of azimuthal divergence and convergence resulting in radial ``spokes'' of convergence. These are not uniformly distinct around the entire circumference but are seen in part of the surrounding area for all 3 sunspots. The angular spacing is about 10 to 20 degrees and the pattern persists for several hours. For one of the sunspots, we have concurrent movies made with a 3 Angstrom wide K line filter. A time average of these images shows bright spokes in the K line congruent with the convergence spokes. Much of the magnetic flux that is continually emerging and moving outward in the moat is in the vicinity of the ``spokes.'' In addition, these data show several good examples of so called ``streakers.'' These are small bright structures seen in continuum movies that appear to be emitted from the outer edge of the penumbral and travel a few thousand km at about 2 to 3 km/s before fading. We find that these are associated with a magnetic field of opposite polarity to the sunspot and that they travel toward another larger and slower moving magnetic feature with the same polarity as the sunspot. When the streaker catches up, it disappears, sometimes coincident with a brightening of the merged feature which continues outward at the previous velocity, about 0.5 km/s. This work was supported by NSF grant ATM-9213879, NASA contracts NAS8-39746 and NAS8-39747, Lockheed Independent Research Funds, and the Swedish Royal Academy of Sciences. Title: Heating of Active Region Corona by Transient Brightenings (Microflares) Authors: Shimizu, T.; Tsuneta, T.; Title, A.; Tarbell, T.; Shine, R.; Frank, Z. Bibcode: 1996mpsa.conf...37S Altcode: 1996IAUCo.153...37S No abstract at ADS Title: New Observations of Subarcsecond Photospheric Bright Points Authors: Berger, T. E.; Schrijver, C. J.; Shine, R. A.; Tarbell, T. D.; Title, A. M.; Scharmer, G. Bibcode: 1995ApJ...454..531B Altcode: We have used an interference filter centered at 4305 Å within the bandhead of the CH radical (the "G band") and real-time image selection at the Swedish Vacuum Solar Telescope on La Palma to produce very high contrast images of subarcsecond photospheric bright points at all locations on the solar disk. During the 6 day period of 1993 September 15-20 we observed active region NOAA 7581 from its appearance on the East limb to a near disk-center position on September 20. A total of 1804 bright points were selected for analysis from the disk center image using feature extraction image processing techniques. The measured FWHM distribution of the bright points in the image is subnormal with a modal value of 220 km (0".30) and an average value of 250 km (0".35). The smallest measured bright point diameter is 120 km (0".17) and the largest is 600 km (0".69). Approximately 60% of the measured bright points are circular (eccentricity ∼1.0), the average eccentricity is 1.5, and the maximum eccentricity corresponding to filigree in the image is 6.5. The peak contrast of the measured bright points is normally distributed. The contrast distribution variance is much greater than the measurement accuracy, indicating a large spread in intrinsic bright-point contrast. When referenced to an averaged "quiet-Sun area 1n the image, the modal contrast is 29% and the maximum value is 75%; when referenced to an average intergranular lane brightness in the image, the distribution has a modal value of 61 % and a maximum of 119%. The bin-averaged contrast of G-band bright points is constant across the entire measured size range. The measured area of the bright points, corrected for population and selection effects, covers about 1.8% of the total image area. Large pores and micropores occupy an additional 2% of the image area, implying a total area fraction of magnetic proxy features in the image of 3.8%. We discuss the implications of this area fraction measurement in the context of previously published measurements which show that typical active region plage has a magnetic filling factor on the order of 10% or greater. The results suggest that in the active region analyzed here, less than 50% of the small-scale magnetic flux tubes are demarcated by visible proxies such as bright points or pores. Title: Simulated MDI Observations of Convection Authors: Hurlburt, N. E.; Schrijver, C. J.; Shine, R. A.; Title, A. M. Bibcode: 1995ESASP.376b.239H Altcode: 1995soho....2..239H; 1995help.confP.239H No abstract at ADS Title: Warning: Local Correlation Tracking may BE Dangerous to your (scientific) Health Authors: Simon, G. W.; Brandt, P. N.; November, L. J.; Shine, R. A.; Strous, L. H. Bibcode: 1995ESASP.376b.223S Altcode: 1995soho....2..223S; 1995help.confP.223S No abstract at ADS Title: The Possible Ascent of a Closed Magnetic System through the Photosphere Authors: Lites, B. W.; Low, B. C.; Martinez Pillet, V.; Seagraves, P.; Skumanich, A.; Frank, Z. A.; Shine, R. A.; Tsuneta, S. Bibcode: 1995ApJ...446..877L Altcode: We present a comprehensive interpretation of the evolution of a small magnetic region observed during its entire disk passage. The vector magnetic field measurements from the Advanced Stokes Polarimeter, along with Hα and magnetogram measurements from the Lockheed SOUP instrument operating at the Swedish Solar Observatory on La Palma, and soft X-ray images from the Yohkoh satellite support the hypothesis that we have observed the passage of a nearly closed magnetic system through the photosphere into the corona. The observations suggest that as the magnetic flux begins to emerge into the photosphere it shows a rather simple geometry, but it subsequently develops a small δ-sunspot configuration with a highly sheared vector field along the polarity inversion line running through it. At that stage, the vector field is consistent with a concave upward magnetic topology, indicative of strong electric currents above the photosphere. An Hα prominence is found above this inversion line when the δ-sunspot is fully formed. These observed features and the sequence of events are interpreted in terms of a nearly closed magnetic system that rises through the photosphere into the corona as a result of magnetic buoyancy. The magnetic system persists in the corona well after the dark δ-sunspot has disappeared in the photosphere We suggest that this coronal structure is in quasi-static equilibrium with its buoyancy partially countered by the weight of the plasma trapped at the bottom of closed magnetic loops. The plausibility of such a scenario is demonstrated by a three-dimensional magnetostatic model of the emergence of a closed, spheroidal magnetic system in the corona, in which the Lorentz force arising from cross-field currents is balanced by the gravitational and pressure forces. This theoretical model carries many features in common with the observed morphology of our active region. Title: Frame Selection Techniques for Solar Movies Authors: Shine, R. A.; Tarbell, T.; Title, A.; Scharmer, G.; Simon, G.; Brandt, P.; Berger, T. Bibcode: 1995SPD....26..506S Altcode: 1995BAAS...27..957S No abstract at ADS Title: Flux Emergence in a Sunspot Moat and Young Active Region Authors: Title, A. M.; Frank, Z. A.; Shine, R. A.; Tarbell, T. D.; Simon, G. W.; Brandt, P. N. Bibcode: 1995SPD....26.1007T Altcode: 1995BAAS...27..978T No abstract at ADS Title: Properties of Sub-Arcsecond Facular Bright Points Authors: Berger, T.; Schrijver, C.; Shine, R.; Tarbell, T.; Title, A.; Scharmer, G. Bibcode: 1995SPD....26..505B Altcode: 1995BAAS...27..957B No abstract at ADS Title: Observations of Convection Authors: Title, A. M.; Hurlburt, N.; Schrijver, C.; Shine, R.; Tarbell, T. Bibcode: 1995ESASP.376a.113T Altcode: 1995heli.conf..113T; 1995soho....1..113T The primary goal of the Solar Oscillations Investigation is to understand the interior of the Sun using the techniques of helioseismology. In addition the Michelson Doppler Imager produces images of the solar surface with sufficient resolution to measure surface flows via the technique of local correlation tracking and magnetograms which allow feature tracking of magnetic fields. It will be possible to measure the evolution of meso and supergranulation, the evolution of the meso and supergranulation patterns, and the motion of magnetic elements in the flow field. With observing periods of 8 hours one should be able to detect large scale flow fields of 10 m/s second or less. The magnetograms will provide the data to understand how the cell patterns evolve as a function of magnetic field configuration. Title: On the Relation Between Facular Bright Points and the Magnetic Field Authors: Berger, Thomas; Shine, Richard; Tarbell, Theodore; Title, Alan; Scharmer, Goran Bibcode: 1994AAS...185.8607B Altcode: 1994BAAS...26.1465B Multi-spectral images of magnetic structures in the solar photosphere are presented. The images were obtained in the summers of 1993 and 1994 at the Swedish Solar Telescope on La Palma using the tunable birefringent Solar Optical Universal Polarimeter (SOUP filter), a 10 Angstroms wide interference filter tuned to 4304 Angstroms in the band head of the CH radical (the Fraunhofer G-band), and a 3 Angstroms wide interference filter centered on the Ca II--K absorption line. Three large format CCD cameras with shuttered exposures on the order of 10 msec and frame rates of up to 7 frames per second were used to create time series of both quiet and active region evolution. The full field--of--view is 60times 80 arcseconds (44times 58 Mm). With the best seeing, structures as small as 0.22 arcseconds (160 km) in diameter are clearly resolved. Post--processing of the images results in rigid coalignment of the image sets to an accuracy comparable to the spatial resolution. Facular bright points with mean diameters of 0.35 arcseconds (250 km) and elongated filaments with lengths on the order of arcseconds (10(3) km) are imaged with contrast values of up to 60 % by the G--band filter. Overlay of these images on contemporal Fe I 6302 Angstroms magnetograms and Ca II K images reveals that the bright points occur, without exception, on sites of magnetic flux through the photosphere. However, instances of concentrated and diffuse magnetic flux and Ca II K emission without associated bright points are common, leading to the conclusion that the presence of magnetic flux is a necessary but not sufficient condition for the occurence of resolvable facular bright points. Comparison of the G--band and continuum images shows a complex relation between structures in the two bandwidths: bright points exceeding 350 km in extent correspond to distinct bright structures in the continuum; smaller bright points show no clear relation to continuum structures. Size and contrast statistical cross--comparisons compiled from measurements of over two-thousand bright point structures are presented. Preliminary analysis of the time evolution of bright points in the G--band reveals that the dominant mode of bright point evolution is fission of larger structures into smaller ones and fusion of small structures into conglomerate structures. The characteristic time scale for the fission/fusion process is on the order of minutes. Title: Flux Emergence in the Sunspot Moat Authors: Title, A. M.; Shine, R. A.; Frank, Z. A.; Simon, G. W.; Brandt, P. N. Bibcode: 1994AAS...185.8602T Altcode: 1994BAAS...26.1464T On 13-15 June 1994 we obtained simultaneous movies of a sunspot in NOAA active region 7731 through a 3 Angstroms band K line filter, the LPARL tunable filter, and an 8 Angstroms G band filter. The data sets allow us to make aligned magnetic, continuum, Doppler, K line, and G band movies. The sunspot had a well developed moat. Flux emergence occured throughout the moat. The initial signature of the emergence was a transient dark elongated structure in the K line images that was aligned radially with respect to the spot. Bright point pairs appeared at the ends of these features in the K line and G band shortly after their emergence. Magnetic field is observed cospatial with the K line bright point pairs. The magnetic polarity of the end of the pair closest to the spot is the same as the spot. The pairs of bright points move across the moat in a radial direction away from the spot. When the pairs reach the moat boundary the leading bright point merges with a moat feature and the two disappear. The leading bright point's field and the moat field cancel, since the moat boundary and the spot have the same polarity. We believe that these features are different from the long observed moving magnetic features associated with sunspots. Title: High-Resolution Observations of the Evershed Effect in Sunspots Authors: Shine, R. A.; Title, A. M.; Tarbell, T. D.; Smith, K.; Frank, Z. A.; Scharmer, Goran Bibcode: 1994ApJ...430..413S Altcode: High spatial resolution movies of sunspots taken at the Swedish Solar Observatory on La Palma reveal that the Evershed effect is time dependent. Outward proper motions are visible in both the continuum and Dopplergrams. These can be tracked over most of the width of the penumbra and overlap regions that show inward moving penubral grains. The radial spacing between the moving structures is about 2000 km, and they exhibit irregular repetitive behavior with a typical interval of 10 minutes. These are probably the cause of 10 minutes oscillations sometimes seen in a penumbral power spectra. Higher velocities are spatially correlated with the relatively darker regions between bright filaments. Regions with a strong variation in the Doppler signal show peak-to-peak modulations of 1 km/s on an average velocity of about 3-4 km/s. The proper motion velocity is approximately constant from the iner penumbra and generally larger than the Doppler velocity when both are interpreted as projections of horizontal motion. Regions where thay are consistent suggest a typical horizontal velocity of 3.5 km/s. Some proper motion velocites as high as 7 km/s are seen, but these are less certain. The temporal behavoir shows a correlation between increased Doppler signal and increased continuum intensity, the opposite of the spatial correlation. When spatially averaged across filaments and over time, the averaged Evershed effect has a peak horizontal component near the outer edge of the penumbra of 2.0 km/s with evidence for a 200-400 m/s upward component. The latter depends on an uncertain absolute velocity calibration. If real it could be an actual upward component or a penumbral analogue of the convective blueshift seen in the quiet Sun. Title: Observing Stellar Coronae with the Goddard High Resolution Spectrograph. I. The dMe Star AU Microscopii Authors: Maran, S. P.; Robinson, R. D.; Shore, S. N.; Brosius, J. W.; Carpenter, K. G.; Woodgate, B. E.; Linsky, J. L.; Brown, A.; Byrne, P. B.; Kundu, M. R.; White, S.; Brandt, J. C.; Shine, R. A.; Walter, F. M. Bibcode: 1994ApJ...421..800M Altcode: We report on an observation of AU Mic taken with the Goddard High Resolution Spectrograph (GHRS) aboard the Hubble Space Telescope. The data consist of a rapid sequence of spectra covering the wavelength range 1345-1375 A with a spectral resolution of 10,000. The observations were originally intended to search for spectral variations during flares. No flares were detected during the 3.5 hr of monitoring. A method of reducing the noise while combining the individual spectra in the time series is described which resulted in the elimination of half of the noise while rejecting only a small fraction of the stellar signal. The resultant spectrum was of sufficient quality to allow the detection of emission lines with an integrated flux of 10-15 ergs/sq cm(sec) or greater. Lines of C I, O I, O V, Cl I, and Fe XXI were detected. This is the first indisputable detection of the 1354 A Fe XXI line, formed at T approximately = 107 K, on a star other than the Sun. The line was well resolved and displayed no significant bulk motions or profile asymmetry. From the upper limit on the observed line width, we derive an upper limit of 38 km/s for the turbulent velocity in the 107 K plasma. An upper limit is derived for the flux of the 1349 A Fe XII line, formed at T approximately = 1.3 x 106 K. These data are combined with contemporaneous GHRS and International Ultraviolet Explorer (IUE) data to derive the volume emission measure distribution of AU Mic over the temperature range 104-107 K. Models of coronal loops in hydrostatic equilibrium are consistent with the observed volume emission measures of the coronal lines. The fraction of the stellar surface covered by the footprints of the loops depends upon the loop length and is less than 14% for lengths smaller than the stellar radius. From the upper limit to the estimated width of the Fe XXI line profile we find that the we cannot rule out Alfven wave dissipation as a possible contributor to the required quiescent loop heating rate. Title: Dynamics of the Evershed effect Authors: Shine, R. A.; Title, A. M.; Tarbell, T. D.; Smith, K.; Frank, Z. A.; Scharmer, G. Bibcode: 1994ASIC..433..197S Altcode: No abstract at ADS Title: On photospheric flows and chromospheric corks Authors: Brandt, P. N.; Rutten, R. J.; Shine, R. A.; Trujillo Bueno, J. Bibcode: 1994ASIC..433..251B Altcode: No abstract at ADS Title: Vector-Stokes polarimetry in a sunspot Authors: Hofmann, A.; Shine, R. A.; Frank, Z. A.; Schmidt, W.; Balthasar, H. Bibcode: 1994smf..conf..204H Altcode: No abstract at ADS Title: High resolution vector polarimetry of sunspot magnetic fields. Authors: Balthasar, H.; Hofmann, A.; Schmidt, W.; Shine, R. A.; Frank, Z. A. Bibcode: 1994AGAb...10..112B Altcode: No abstract at ADS Title: Large-scale photospheric motions: first results from an extraordinary eleven-hour granulation observation Authors: Simon, G. W.; Brandt, P. N.; November, L. J.; Scharmer, G. B.; Shine, R. A. Bibcode: 1994ASIC..433..261S Altcode: No abstract at ADS Title: High Resolution Observations of the Evershed Flow in Sunspots Authors: Shine, R.; Title, A.; Smith, K.; Scharmer, G. Bibcode: 1993BAAS...25.1183S Altcode: No abstract at ADS Title: Multitemperature Observations of an Emerging Flux Region Authors: Bruner, M. E.; Acton, L. W.; Brown, W. A.; Lemen, J. R.; Shine, R.; Strong, K. T.; Tarbell, T.; Dulk, G.; Tsuneta, S.; Bastian, T.; Dame, L. Bibcode: 1993BAAS...25.1179B Altcode: No abstract at ADS Title: Observations of an Emerging Flux Region Authors: Brown, W. A.; Acton, L. W.; Bruner, M. E.; Lemen, J. R.; Shine, R.; Strong, K. T.; Tarbell, T.; Dulk, G.; Tsuneta, S.; Bastian, T.; Dame, L. Bibcode: 1993BAAS...25Q1214B Altcode: No abstract at ADS Title: Solar Coronal Magnetic Field Topology Inferred from High Resolution Optical and X-ray Movies Authors: Tarbell, T.; Frank, Z.; Hurlburt, N.; Morrison, M.; Shine, R.; Title, A.; Acton, L. Bibcode: 1993BAAS...25.1208T Altcode: No abstract at ADS Title: La Palma Observations During the CoMStOC'92 Campaign Authors: Shine, R.; Tarbell, T.; Topka, K.; Frank, Z.; Title, A.; Scharmer, G. Bibcode: 1993BAAS...25S1223S Altcode: No abstract at ADS Title: ``The Active Sun'': Educational Videotapes on Solar Physics for College Astronomy Authors: Hurlburt, N.; Title, A.; Tarbell, T.; Frank, Z.; Topka, K.; Shine, R. Bibcode: 1993AAS...182.1002H Altcode: 1993BAAS...25..809H We present a series of short, educational documentaries on solar physics aimed at college-level general astronomy courses. These tapes highlight recent advances in high-resolution solar astronomy and in theoretical and computational modeling of solar physics with particular focus on dynamical phenomena. The relevant physical mechanisms, theoretical interpretations and observational techniques are discussed. These include granulation, the theory of convection, five-minute oscillations, sunspots, magnetic fields, seeing and dopplergrams. VHS tapes are available to researchers and educators through a variety of distributors. This work supported by Lockheed Independent Research Funds. Title: Solar Coronal Magnetic Field Topology Inferred from High Resolution Optical and X-ray Movies Authors: Tarbell, T.; Frank, Z.; Hurlburt, N.; Morrison, M.; Shine, R.; Title, A.; Acton, L. Bibcode: 1993AAS...182.4805T Altcode: 1993BAAS...25R.880T We are using high resolution digital movies of solar active regions in optical and X-ray wavelengths to study solar flares and other transients. The optical movies were collected at the Swedish Solar Observatory on La Palma using the Lockheed tunable filtergraph system, in May - July, 1992. They include longitudinal and transverse magnetograms, H-alpha Doppler and intensity images at many wavelengths, Ca K, Na D, and white light images. Simultaneous X-ray images from Yohkoh are available much of the time. We are learning several ways to establish the connectivity of some coronal magnetic field lines. Some of the clues available are: magnetic footpoint polarities and transverse field directions; H-alpha fibrils and loops seen in several wavelengths; proper motion and Doppler shifts of blobs moving along field lines; footpoint brightening in micro-flares; spreading of flare ribbons during gradual phases of flares; X-ray morphology and correlations with H-alpha; and draining of flare loops. Examples of each of these will be shown on video. This work is supported by NASA Contracts NASW-4612 and NAS8-37334 and by Lockheed Independent Research Funds. Title: On the Magnetic and Velocity Field Geometry of Simple Sunspots Authors: Title, Alan M.; Frank, Zoe A.; Shine, Richard A.; Tarbell, Theodore D.; Topka, Kenneth P.; Scharmer, Goran; Schmidt, Wolfgang Bibcode: 1993ApJ...403..780T Altcode: It is presently shown that a simple sunspot model with azimuthal variations in inclination, but lacking azimuthal field-strength variations, is free from azimuthal Lorentz forces. The meridional currents arising from the inclination variations are parallel to the field lines, suggesting that a cylindrically symmetric magnetostatic sunspot model can be perturbed into one with azimuthal variations in inclination with adjustment of the meridional force balance. Title: White-light movies of the solar photosphere from the SOUP instrument on Spacelab 2 (Advances in Space Research 1986) Authors: Title, A. M.; Tarbell, T. D.; Simon, G. W.; Acton, L.; Duncan, D.; Ferguson, S.; Finch, M.; Frank, Z.; Kelly, G.; Lindgren, R.; Morrill, M.; Pope, T.; Reeves, R.; Rehse, R.; Shine, R.; Topka, K.; Harvey, J.; Leibacher, J.; Livingston, W.; November, L. Bibcode: 1993inas.book..100T Altcode: No abstract at ADS Title: Data Compression Experiments with High Resolution Solar Images Authors: Shine, R. A.; Majani, E. E. Bibcode: 1992AAS...181.8113S Altcode: 1992BAAS...24.1254S No abstract at ADS Title: High resolution observations: the state of the art and beyond. Authors: Title, A.; Tarbell, T.; Shine, R.; Topka, K.; Frank, Z. Bibcode: 1992ESASP.344....9T Altcode: 1992spai.rept....9T Excellent telescopes on excellent sites with fast digital CCD cameras and special purpose computers allow the collection of broad band images at just the instants of good seeing. This has resulted in nearly optimal movies of the solar surface for several hours. When longer exposures are required for narrowband filtergrams or spectra it is not enough to capture single images. However, big fast memories allow the collection of many selected low signal-to-noise ratio images in real time, which can be summed to achieve the desired signal to noise ratios. Adaptive optics shows promise of diffraction limited images for limited fields of view. Nevertheless, groundbased observations will always be limited in their duration, uniformity, and resolution qualities which are essential for understanding the development and evolution of small scale processes. Until there are observations in space we will not be able to completely understand either the processes in the solar atmosphere or how processes occurring at different height are interrelated. Title: Evolution and advection of solar mesogranulation Authors: Muller, Richard; Auffret, Herve; Roudier, Thierry; Vigneau, Jean; Simon, George W.; Frank, Zoe; Shine, Richard A.; Title, Alan M. Bibcode: 1992Natur.356..322M Altcode: GRANULAR structure on the Sun's surface, with a typical scale of 1-2 Mm, has been known since 1800, and one hundred years ago, with the first observations by spectroheliograph1,2, a mesh-like bright network was found with a characteristic scale of 30 Mm (40''). This pattern was found, thirty years ago, to be coincident with close-packed convective cells ('supergranulation') revealed by Doppler observations3-5 to be nestling inside the bright network. More recently6,7 an intermediate 'mesogranular' structure was found, with a characteristic scale of 3-10 Mm. We have obtained a three-hour sequence of observations at the Pic du Midi observatory which shows the evolution of mesogranules from appearance to disappearance with unprecedented clarity. We see that the supergranules, which are known to carry along (advect) the granules with their convective motion, also advect the mesogranules to their boundaries. This process controls the evolution and disappearance of mesogranules. Title: High Resolution Observations of the Magnetic and Velocity Field of Simple Sunspots Authors: Title, Alan M.; Frank, Zoe A.; Shine, Richard A.; Tarbell, T. D.; Topka, K. P.; Scharmer, Goran; Schmidt, Wolfgang Bibcode: 1992ASIC..375..195T Altcode: 1992sto..work..195T We have observed the disk passage of relatively simple round sunspots using a narrowband filter and a large format CCD detector and have created magnetograms, Dopplergrams, and continuum images nearly simultaneously. In addition the spectral resolution of the filter allows the construction of 'spectra' for all points in the field of view. The mean inclination of the magnetic field increases from 45-50 deg to 70-75 deg across the penumbra and there is a fluctuation of the inclination angle about the mean of about 4 +/- 18 deg. The variation in inclination is large enough that substantial amounts of magnetic field are parallel to the solar surface from the mid to outer penumbra. The Evershed flow tends to occur in the regions where the magnetic field is horizontal. This suggests that the Evershed flow is confined to the regions of horizontal fields. We show that a simple sunspot model with azimuthal variations in inclination but no azimuthal variations of field strength is free from azimuthal Lorentz forces. The meridional component of the currents which arise from the azimuthal variation in inclination are parallel to the field lines. This suggests that a cylindrically symmetric magnetostatic sunspot model can be perturbed into one with azimuthal variations in inclination with some adjustment in the meridional force balance. Title: Dynamics of the Quiet Solar Atmosphere: K2v Cell Grains Versus Magnetic Elements Authors: Brandt, P. N.; Rutten, R. J.; Shine, R. A.; Trujillo Bueno, J. Bibcode: 1992ASPC...26..161B Altcode: 1992csss....7..161B No abstract at ADS Title: An Investigation of the Flare Star AU Mic with the Goddard High Resolution Spectrograph on the Hubble Space Telescope Authors: Maran, S. P.; Woodgate, B. E.; Carpenter, K. G.; Robinson, R. D.; Shore, S. N.; Linsky, J. L.; Brown, A.; Byrne, P. B.; Kundu, M. R.; White, S.; Brandt, J. C.; Shine, R. A.; Walter, F. M. Bibcode: 1991BAAS...23.1382M Altcode: No abstract at ADS Title: Observations of the Birth and Death of Mesogranules Authors: Simon, G. W.; Title, A. M.; Shine, R. A.; Frank, Z.; Muller, R.; Auffret, H. Bibcode: 1991BAAS...23.1034S Altcode: No abstract at ADS Title: Field Geometry of Sunspots Inferred from Inclination Effects Authors: Title, A. M.; Frank, Z. A.; Shine, R. A.; Tarbell, T. D. Bibcode: 1991BAAS...23R1052T Altcode: No abstract at ADS Title: Sunspot Umbral and Penumbral Oscillations in Hα Authors: Shine, R.; Tarbell, T.; Title, A.; Topka, K.; Frank, Z.; Smith, K. Bibcode: 1991BAAS...23.1033S Altcode: No abstract at ADS Title: Variation of granulation properties on a mesogranular scale Authors: Brandt, P. N.; Ferguson, S.; Shine, R. A.; Tarbell, T. D.; Scharmer, G. B. Bibcode: 1991A&A...241..219B Altcode: A 79 min series of CCD images of the solar granulation with subarcsec spatial resolution is analyzed. Local correlation techniques are applied to determine horizontal displacements of the granular intensity pattern in a 14.2 by 12.2 sq arcsec field of view. The divergence of the average horizontal flow field shows mean cell sizes of 5 to 7 arcsec. Granules are selected with respect to area, brightness, lifetime, and expansion rate. It is shown that small, faint, short-lived, and fast collapsing granules are located preferentially in the negative divergence (down-draft) regions of the mesogranular flow field, while bright, long-lived, and rapidly expanding granules populate preferentially the positive divergence (up-draft) regions. The differences in area coverage range between + or - 6 percent and + or - 9 percent. Title: Results from high resolution solar images and spectra obtained at the Pic du Midi Observatory (1986-1990) Authors: Roudier, Th.; Muller, R.; Vigneau, J.; Auffret, H.; Espagnet, O.; Simon, G. W.; Title, A. M.; Frank, Z.; Shine, R. A.; Tarbell, T. D.; Mein, P.; Malherbe, J. M. Bibcode: 1991AdSpR..11e.205R Altcode: 1991AdSpR..11..205R We present an overview of our recent results about solar granulation and mesogranulation, obtained with Pic du Midi observations. These results were obtained during 1986-1990 using image and spectrographic analysis of high spatial resolution data. The study of the solar granulation, with 2 Dim. ``Multichannel Subtractive Double Pass'' (M.S.D.P.) spectra, shows a clear change of the dynamical regime at 3'' (⋍ 2200 km) of the photospheric velocity field when oscillatory components are filtered out.

A three hour movie obtained on film at Pic du Midi Observatory and analyzed at the Lockheed Research Laboratory and the National Solar Observatory (Sacramento Peak) was used to calculate the horizontal flow pattern. The mean lifetime of the diverging areas related to mesogranulation is estimated at 3 hours; these diverging areas are swept by the supergranulation flow towards the supergranule boundary with a mean speed of 0.4 km/s. Title: Generation of Electric Currents and Waves on Magnetic Flux Tubes by Horizontal Velocities in the Photosphere (With 1 Figure) Authors: Tarbell, T. D.; Slater, G. L.; Frank, Z. A.; Shine, R. A.; Topka, K. P. Bibcode: 1991mcch.conf...39T Altcode: No abstract at ADS Title: SOUP Observations of Solar Activity Authors: Shine, R. A.; Scharmer, G.; Tarbell, T. D.; Title, A. M.; Topka, K. P. Bibcode: 1991max..conf..295S Altcode: No abstract at ADS Title: Detailed Comparison of Quiet and Magnetic Sun Authors: Topka, K.; Ferguson, S.; Shine, R.; Tarbell, T.; Title, A.; Balke, C.; Scharmer, G.; Schmidt, W. Bibcode: 1990BAAS...22R.879T Altcode: No abstract at ADS Title: Penumbral Flows and Magnetic Fields Authors: Shine, R.; Smith, K.; Tarbell, T.; Title, A.; Scharmer, G. Bibcode: 1990BAAS...22..878S Altcode: No abstract at ADS Title: Generation of Waves and Electric Currents on Magnetic Flux Tubes by Horizontal and Vertical Velocities in the Photosphere Authors: Frank, Z. A.; Shine, R. A.; Slater, G.; Tarbell, T.; Topka, K. Bibcode: 1990BAAS...22..878F Altcode: No abstract at ADS Title: High-Resolution Observations of Emerging Magnetic Fields and Flux Tubes in Active Region Photosphere Authors: Tarbell, T.; Ferguson, S.; Frank, Z.; Shine, R.; Title, A.; Topka, K.; Scharmer, G. Bibcode: 1990IAUS..138..147T Altcode: No abstract at ADS Title: Structure and Evolution of the Large Scale Granulation Authors: Muller, R.; Roudier, Th.; Vigneau, J.; Frank, Z.; Shine, R.; Tarbell, T.; Title, A.; Simon, G. Bibcode: 1990PDHO....7...44M Altcode: 1990dysu.conf...44M; 1990ESPM....6...44M A granulation movie of 3 hours has been performed at the Pic du Midi Observatory on September 20, 1988. Title: High Resolution Observations of the Photosphere Authors: Title, A. M.; Shine, R. A.; Tarbell, T. D.; Topka, K. P.; Scharmer, G. B. Bibcode: 1990IAUS..138...49T Altcode: No abstract at ADS Title: Formation of Network Bright Points by Granule Compression Authors: Muller, R.; Roudier, Th.; Vigneau, J.; Frank, Z.; Shine, R.; Tarbell, T.; Title, A.; Simon, G. Bibcode: 1990PDHO....7..150M Altcode: 1990dysu.conf..150M; 1990ESPM....6..150M No abstract at ADS Title: Intial Results of the Lockheed 1989 La Palma Observing Campaign Authors: Topka, K.; Frank, Z.; Shine, R.; Smith, K.; Tarbell, T.; Title, A.; Scharmer, G. Bibcode: 1989BAAS...21.1111T Altcode: No abstract at ADS Title: Variation of granulation properties on a meso-granular scale Authors: Brandt, P. N.; Ferguson, S.; Scharmer, G. B.; Shine, R. A.; Tarbell, T. D.; Title, A. M.; Topka, K. Bibcode: 1989hsrs.conf..473B Altcode: No abstract at ADS Title: Proper Motion and Lifetime of Mesogranules Authors: Frank, Z.; Muller, R.; Roudier, T.; Vigneau, J.; Shine, R.; Tarbell, T.; Title, A.; Topka, K.; Simon, G. Bibcode: 1989BAAS...21..841F Altcode: No abstract at ADS Title: Short Term Evolution of Fine Scale Magnetic Structures Authors: Topka, K.; Frank, Z.; Shine, R.; Tarbell, T.; Title, A.; Scharmer, G.; Balke, A. Bibcode: 1989BAAS...21..842T Altcode: No abstract at ADS Title: Magnetic Field Inclination in Penumbra of a Round Sunspot Observed at Very High Spatial Resolution Authors: Title, A. M.; Frank, Z. A.; Shine, R. A.; Tarbell, T. D.; Scharmer, G. Bibcode: 1989BAAS...21Q.837T Altcode: No abstract at ADS Title: Investigation of Active Regions at High Resolution by Balloon Flights of the Solar Optical Universal Polarimeter (SOUP) Authors: Tarbell, T.; Gilbreth, C.; Shine, R.; Title, A.; Topka, K.; Wolfson, J. Bibcode: 1989BAAS...21R.837T Altcode: No abstract at ADS Title: Observations of Running Penumbral Waves Authors: Shine, R.; Tarbell, T.; Title, A.; Topka, K.; Frank, Z.; Scharmer, G. Bibcode: 1989BAAS...21..837S Altcode: No abstract at ADS Title: Generation of Waves on Magnetic Flux Tubes by Horizontal Velocities in the Photosphere Authors: Tarbell, T. D.; Ferguson, S. H.; Frank, Z. A.; Shine, R. A. Bibcode: 1989BAAS...21..830T Altcode: No abstract at ADS Title: Details of Large Scale Solar Motions Revealed by Granulation Test Particles Authors: Simon, G. W.; November, L. J.; Ferguson, S. H.; Shine, R. A.; Tarbell, T. D.; Title, A. M.; Topka, K. P.; Zirin, H. Bibcode: 1989ASIC..263..371S Altcode: 1989ssg..conf..371S No abstract at ADS Title: Statistical Properties of Solar Granulation Derived from the SOUP Instrument on Spacelab 2 Authors: Title, A. M.; Tarbell, T. D.; Topka, K. P.; Ferguson, S. H.; Shine, R. A.; SOUP Team Bibcode: 1989ApJ...336..475T Altcode: Computer algorithms and statistical techniques were used to identify, measure, and quantify the properties of solar granulation derived from movies collected by the Solar Optical Universal Polarimeter on Spacelab 2. The results show that there is neither a typical solar granule nor a typical granule evolution. A granule's evolution is dependent on local magnetic flux density, its position with respect to the active region plage, its position in the mesogranulation pattern, and the evolution of granules in its immediate neighborhood. Title: Flows, Random Motions and Oscillations in Solar Granulation Derived from the SOUP Instrument on Spacelab 2 Authors: Title, A. M.; Tarbell, T. D.; Topka, K. P.; Ferguson, S. H.; Shine, R. A.; SOUP Team Bibcode: 1989ASIC..263..225T Altcode: 1989ssg..conf..225T No abstract at ADS Title: Magnetoconvection on the solar surface. Authors: Simon, G. W.; Title, A. M.; Topka, K. P.; Tarbell, T. D.; Shine, R. A.; Ferguson, S. H.; Zirin, H. Bibcode: 1989GMS....54...53S Altcode: 1989sspp.conf...53S The authors describe and illustrate the first high-resolution observations of horizontal flows on the solar surface and their relation to magnetic field structure seen in the Sun's photosphere. Title: Chromospheric explosions. Authors: Doschek, G. A.; Antiochos, S. K.; Antonucci, E.; Cheng, C. -C.; Culhane, J. L.; Fisher, G. H.; Jordan, C.; Leibacher, J. W.; MacNiece, P.; McWhirter, R. W. P.; Moore, R. L.; Rabin, D. M.; Rust, D. M.; Shine, R. A. Bibcode: 1989epos.conf..303D Altcode: The work of this team addressed the question of the response and relationship of the flare chromosphere and transition region to the hot coronal loops that reach temperatures of about 107K and higher. Flare related phenomena such as surges and sprays were also discussed. The team members debate three main topics: 1) whether the blue-shifted components of X-ray spectral lines are signatures of "chromospheric evaporation"; 2) whether the excess line broadening of UV and X-ray lines is accounted for by "convective velocity distribution" in evaporation; and 3) whether most chromospheric heating is driven by electron beams. These debates illustrated the strengths and weaknesses of our current observations and theories. Title: Vortex Motion of the Solar Granulation Authors: Brandt, P. N.; Scharmer, G. B.; Ferguson, S. H.; Shine, R. A.; Tarbell, T. D.; Title, A. M. Bibcode: 1989ASIC..263..305B Altcode: 1989ssg..conf..305B No abstract at ADS Title: Investigation of active regions at high resolution by balloon flights of the Solar Optical Universal Polarimeter (SOUP) Authors: Tarbell, T.; Frank, Z.; Gilbreth, C.; Shine, R.; Title, A.; Topka, K.; Wolfson, J. Bibcode: 1989dots.work..310T Altcode: SOUP is a versatile, visible-light solar observatory, built for space or balloon flight. It is designed to study magnetic and velocity fields in the solar atmosphere with high spatial resolution and temporal uniformity, which cannot be achieved from the surface of the earth. The SOUP investigation is carried out by the Lockheed Palo Alto Research Laboratory, under contract to NASA's Marshall Space Flight Center. Co-investigators include staff members at a dozen observatories and universities in the U.S. and Europe. The primary objectives of the SOUP experiment are: to measure vector magnetic and velocity fields in the solar atmosphere with much better spatial resolution than can be achieved from the ground; to study the physical processes that store magnetic energy in active regions and the conditions that trigger its release; and to understand how magnetic flux emerges, evolves, combines, and disappears on spatial scales of 400 to 100,000 km. SOUP is designed to study intensity, magnetic, and velocity fields in the photosphere and low chromosphere with 0.5 arcsec resolution, free of atmospheric disturbances. The instrument includes: a 30 cm Cassegrain telescope; an active mirror for image stabilization; broadband film and TV cameras; a birefringent filter, tunable over 5100 to 6600 A with 0.05 A bandpass; a 35 mm film camera and a digital CCD camera behind the filter; and a high-speed digital image processor. Title: Observations of f- and p-mode oscillations of high degree (500 < l < 2500) in quiet and active Sun. Authors: Tarbell, T. D.; Peri, M.; Frank, Z.; Shine, R.; Title, A. M. Bibcode: 1988ESASP.286..315T Altcode: 1988ssls.rept..315T Spectra (l-ν diagrams) from high resolution observations taken at the Vacuum Tower Telescope (NSO/Sunspot) are presented. The raw data are CCD images taken through the SOUP narrowband filter in Fe I 5576 Å. Four filtergrams spaced through the spectral line are combined to form velocity movies. Spectra for 80 minutes of data with 0.5 - 1.5 arcsecond resolution are presented for the entire field-of-view and for quiet and magnetic (plage) subregions. Ridges f and p1 - p5 are evident in velocity spectra, extending to l = 2500(f), l = 1800(p1), and l = 1200(p2). Much less power is seen in the magnetic region than in the quiet sun. Three-dimensional Fourier filtering shows that oscillation velocity amplitude drops sharply at the boundary of the active region for each family of modes considered. Title: Active region evolution in the chromosphere and transition region Authors: Shine, R. A.; Schrijver, C. J. Bibcode: 1988fnsm.work...29S Altcode: Images in the C IV 1548 A and the Si II 1526 S lines taken with the ultraviolet spectrometer polarimeter (UVSP) instrument on board the Solar Maximum Mission (SMM) satellite were combined into movies showing the evolution of active regions and the neighboring supergranulation over several days. The data sets generally consist of 240 by 240 arc second rasters with 3 arc second pixels taken one per orbit (about every 90 minutes). The images are projected on a latitude/longitude grid to remove the forshortening as the region rotates across the solar disk and further processed to remove jitter and gain variations. Movies were made with and without differential rotation. Although there are occasional missing orbits, these series do not suffer from the long nighttime gaps that occur in observations taken at a single groundbased observatory and are excellent for studying changes on time scales of several hours. The longest sequence processed to date runs from 20 Oct. 1980 to 25 Oct. 1980. This was taken during an SMM flare buildup study on AR 2744. Several shorter sequences taken in 1980 and 1984 will also be shown. The results will be presented on a video disk which can be interactively controlled to view the movies. Title: Statistical properties of solar granulation from the SOUP instrument on Spacelab 2 Authors: Topka, K.; Title, A.; Tarbell, T.; Ferguson, S.; Shine, R. Bibcode: 1988fnsm.work..294T Altcode: The Solar Optical Universal Polarimeter (SOUP) on Spacelab 2 collected movies of solar granulation completely free from atmospheric blurring, and are not degraded by pointint jitter (the pointing stability was 0.003 sec root mean square). The movies illustrate that the solar five minute oscillation has a major role in the appearance of solar granulation and that exploding granules are a common feature of the granule evolution. Using 3-D Fourier filtering techniques the oscillations were removed and it was demonstrated that the autocorrelation lifetime of granulation is a factor of two greater in magnetic field regions than in field-free quiet sun. Horizontal velocities were measured and flow patterns were observed on the scale of meso- and super granulation. In quiet regions the mean flow velocity is 370 m/s while in the magnetic regions it is about 125 m/s. It was also found that the root mean square (RMS) fluctuating horizonal velocity field is substantially greater in quiet sun than in strong magnetic field regions. By superimposing the location of exploding granules on the average flow maps it was found that they appear almost exclusively in the center of mesogranulation size flow cells. Because of the nonuniformity of the distribution of exploding granules, the evolution of the granulation pattern in mesogranule cell centers and boundaries differs fundamentally. It is clear from this study there is neither a typical granule nor a typical granule evolution. Title: Observations of Granulation in Quiet and Magnetic Sun from the Swedish Solar Observatory on LaPalma Authors: Topka, K.; Ferguson, S.; Frank, Z.; Shine, R.; Tarbell, T.; Title, A.; Wolfson, J.; Scharmer, G.; Brandt, P. Bibcode: 1988BAAS...20S1010T Altcode: No abstract at ADS Title: Solar Activity and Flare Observations from the Swedish Solar Observatory on La Palma Authors: Wolfson, J.; Ferguson, S.; Frank, Z.; Shine, R.; Tarbell, T.; Title, A.; Topka, K.; Scharmer, G.; Brandt, P.; Gurman, J. Bibcode: 1988BAAS...20..978W Altcode: No abstract at ADS Title: Vortex flow in the solar photosphere Authors: Brandt, P. N.; Scharmer, G. B.; Ferguson, S.; Shine, R. A.; Tarbell, T. D.; Title, A. M. Bibcode: 1988Natur.335..238B Altcode: Convective flow fields in the solar atmosphere play a key role in the concentration and dispersal of magnetic flux1, but because the individual flow elements-the solar granules-are a few arcsec or less in size, studies of their motions have been limited by the distortion and blurring of the Earth's atmosphere ('seeing'). We report here a very high-quality series of granulation images taken at the new Swedish Solar Observatory on La Palma (Canary Islands) which have permitted flow measurements at the sub-arcsec level. These movies show a vortex structure which visibly dominates the motion of the granules in its neighbourhood and persists for the 1.5 h duration of the movie. If such vortices are a common feature of the solar convective zone, they may provide an important mechanism for the heating of stellar chromospheres and coronae by twisting the footprints of magnetic flux tubes. Title: On the Relation between Photospheric Flow Fields and the Magnetic Field Distribution on the Solar Surface Authors: Simon, George W.; Title, A. M.; Topka, K. P.; Tarbell, T. D.; Shine, R. A.; Ferguson, S. H.; Zirin, H.; SOUP Team Bibcode: 1988ApJ...327..964S Altcode: Using the technique of local correlation tracking on a 28 minute time sequence of white-light images of solar granulation, the horizontal flow field on the solar surface is measured. The time series was obtained by the Solar Optical Universal Polarimeter (SOUP) on Spacelab 2 (Space Shuttle flight 51-F) and is free from atmospheric blurring and distortion. The SOUP flow fields have been compared with carefully aligned magnetograms taken over a nine hour period at the Big Bear Solar Observatory before, during, and after the SOUP images. The flow field and the magnetic field agree in considerable detail: vectors which define the flow of the white-light intensity pattern (granulation) point toward magnetic field regions, magnetic fields surround flow cells, and magnetic features move along the flow arrows. The projected locations of free particles ('corks') in the measured flow field congregate at the same locations where the magnetic field is observed. Title: Observations of F-and P-Mode Oscillations of High Degree (500< <3500) in Quiet and Active Sun Authors: Peri, M.; Frank, Z.; Shine, R.; Tarbell, T.; Title, A. Bibcode: 1988BAAS...20..702P Altcode: No abstract at ADS Title: Active Region Evolution in the Chromosphere and Transition Region Authors: Shine, R. A.; Schrijver, C. Bibcode: 1988BAAS...20..744S Altcode: No abstract at ADS Title: Solar Granulation Movies of Exceptional Spatial Resolution: Observations and Simulations of Horizontal Convective Flows Authors: Title, A.; Shine, R.; Ferguson, S.; Tarbell, T.; Brandt, P.; Scharmer, G. Bibcode: 1988BAAS...20R.679T Altcode: No abstract at ADS Title: Statistical Properties of Solar Granulation from the SOUP Instrument on Spacelab 2 Authors: Topka, K.; Title, A.; Tarbell, T.; Ferguson, S.; Shine, R. Bibcode: 1988BAAS...20Q.679T Altcode: No abstract at ADS Title: Variability of solar mesogranulation Authors: Simon, G. W.; November, L. J.; Acton, L. W.; Ferguson, S. H.; Shine, R. A.; Tarbell, T. D.; Title, A. M.; Topka, K. P.; Zirin, H. Bibcode: 1988AdSpR...8g.169S Altcode: 1988AdSpR...8..169S From white-light photographs of solar granulation obtained with the SOUP instrument on Space Shuttle Flight STS-19 we have measured the motions of granules using local correlation tracking techniques. The granules are organized into larger-scale structures (mesogranular and supergranular) which exhibit outflow from upwellings, convergence into sinks, as well as significant vorticity. Magnetic fields follow these same flow patterns. We describe these velocity structures, and suggest that their effect on magnetic field structures may be important to the solar flare buildup process. Title: Correlation Lifetimes of Quiet and Magnetic Granulation from the SOUP Instrument on Spacelab 2 Authors: Title, A.; Tarbell, T.; Topka, K.; Acton, L.; Duncan, D.; Ferguson, S.; Finch, M.; Frank, Z.; Kelly, G.; Lindgren, R.; Morrill, M.; Pope, T.; Reeves, R.; Rehse, R.; Shine, R.; Simon, G.; Harvey, J.; Leibacher, J.; Livingston, W.; November, L.; Zirker, J. Bibcode: 1988ApL&C..27..141T Altcode: The time sequences of diffraction limited granulation images obtained by the Solar Optical Universal Polarimeter on Spacelab 2 are presented. The uncorrection autocorrelation limetime in magnetic regions is dominated by the 5-min oscillation. The removal of this oscillation causes the autocorrelation lifetime to increase by more than a factor of 2. The results suggest that a significant fraction of granule lifetimes are terminated by nearby explosions. Horizontal displacements and transverse velocities in the intensity field are measured. Lower limits to the lifetime in the quiet and magnetic sun are set at 440 s and 950 s, respectively. Title: The relation between convection flows and magnetic structure at the solar surface Authors: Simon, G. W.; November, L. J.; Acton, L. W.; Title, A. M.; Tarbell, T. D.; Topka, K. P.; Shine, R. A.; Ferguson, S. H.; Weiss, N. O.; Zirin, H. Bibcode: 1988AdSpR...8k.133S Altcode: 1988AdSpR...8..133S We describe recent results from the comparison of data from the Solar Optical Universal Polarimeter instrument on Spacelab 2 and magnetograms from Big Bear Solar Observatory. We show that the Sun's surface velocity field governs the structure of the observed magnetic field over the entire solar surface outside sunspots and pores. We attempt to describe the observed flows by a simple axisymmetric plume model. Finally, we suggest that these observations may have important implications for the prediction of solar flares, mass ejections, and coronal heating. Title: White Light Sunspot Observations from the Solar Optical Universal Polarimeter on Spacelab-2 Authors: Shine, R. A.; Title, A. M.; Tarbell, T. D.; Topka, K. P. Bibcode: 1987Sci...238.1264S Altcode: The flight of the Solar Optical Universal Polarimeter on Spacelab-2 provided the opportunity for the collection of time sequences of diffraction-limited (0.5 arc second) solar images with excellent pointing stability (0.003 arc second) and with freedom from the distortion that plagues ground-based images. A series of white-light images of active region 4682 were obtained on 5 August 1985, and the area containing the sunspot has been analyzed. These data have been digitally processed to remove noise and to separate waves from low-velocity material motions. The results include (i) proper motion measurements of a radial outflow in the photospheric granulation pattern just outside the penumbra; (ii) discovery of occasional bright structures (``streakers'') that appear to be ejected outward from the penumbra; (iii) broad dark ``clouds'' moving outward in the penumbra, in addition to the well-known bright penumbral grains moving inward; (iv) apparent extensions and contractions of penumbral filaments over the photosphere; and (v) observation of a faint bubble or looplike structure that seems to expand from two bright penumbral filaments into the photosphere. Title: Vortex Flow in Granulation Authors: Scharmer, G.; Brandt, P.; Title, A.; Shine, R.; Ferguson, S. Bibcode: 1987BAAS...19Q1118S Altcode: No abstract at ADS Title: High-Resolution CCD Observations of Doppler and Magnetic Images in the Solar Photosphere Authors: Tarbell, T. D.; Frank, Z. A.; Morrill, M. E.; Shine, R. A.; Topka, K. P.; Title, A. M. Bibcode: 1987BAAS...19.1117T Altcode: No abstract at ADS Title: Sunspot observations from the SOUP instrument on Spacelab 2. Authors: Shine, R. A.; Title, A. M.; Tarbell, T. D.; Acton, L.; Duncan, D.; Ferguson, S. H.; Finch, M.; Frank, Z.; Kelly, G.; Lindgren, R. Bibcode: 1987NASCP2483..133S Altcode: 1987tphr.conf..133S A series of white light images obtained by the SOUP instrument on Spacelab 2 of active region 4682 on August 5, 1985 were analyzed in the area containing sunspots. Although the umbra of the spot is underexposed, the film is well exposed in the penumbral regions. These data were digitally processed to remove noise and to separate p-mode oscillations from low velocity material motions. The results of this preliminary investigation include: (1) proper motion measurements of a radial outflow in the photospheric granulation pattern just outside the penumbra; (2) discovery of occasional bright structures (streakers) that appear to be ejected outward from the penumbra; (3) broad dark clouds moving outward in the penumbra in addition to the well known bright penumbral grains moving inward; (4) apparent extensions and contractions of penumbral filaments over the photosphere; and (5) observation of a faint bubble or loop-like structure which seems to expand from two bright penumbral filaments into the photosphere. Title: Simultaneous Sunspot Observations from the SOUP Instrument on Spacelab 2 and the Big Bear Solar Observatory Authors: Shine, R. A.; Title, A. M.; Topka, K. P.; Tarbell, T. D.; Zirin, H. Bibcode: 1987BAAS...19..927S Altcode: No abstract at ADS Title: Ocean Waves in the Photosphere: Measurements of Oscillations with Wavelengths of 1 - 10 Mm from SOUP White Light Images Authors: Tarbell, T. D.; Shine, R. A.; Ferguson, S. H.; Title, A. M.; Leibacher, J. W. Bibcode: 1987BAAS...19Q.936T Altcode: No abstract at ADS Title: New Ideas About Granulation Based on Data from the Solar Optical Universal Polarimeter Instrument on Spacelab 2 and Magnetic Data from Big Bear Solar Observatory Authors: Title, A. M.; Tarbell, T. D.; Topka, K. P.; Shine, R. A.; Simon, G. W.; Zirin, H.; SOUP Team Bibcode: 1987LNP...292..173T Altcode: 1987ssp..conf..173T The SOUP flow fields have been compared with carefully aligned magnetograms taken at the BBSO before, during, and after the SOUP images. The magnetic field is observed to exist in locations where either the flow is convergent or on the boundaries of the outflow from a flow cell center. Streamlines calculated from the flow field agree very well with the observed motions of the magnetic field in the BBSO magnetogram movies. Title: SMM Observations of SI IV and O IV Bursts in Solar Active Regions Authors: Hayes, Marion; Shine, R. A. Bibcode: 1987ApJ...312..943H Altcode: Observations of Si IV and O IV lines in solar active regions taken by the ultraviolet spectrometer and polarimeter on board the SMM are analyzed. The average frequency of UV bursts of all types is one every four minutes in a 28 arcsec by 28 arcsec field of view. About 80 percent of the bursts show an increased Si IV/O IV ratio, suggesting a density increase. The indicated electron densities are generally in the 10 to the 11th-12th range, with 16 percent indicating higher densities. Some of the more energetic bursts exhibit flarelike characteristics, and some of these show a secondary brightening which may be an analog of the soft X-ray gradual phase of flares. The high frequency of these UV bursts and their possible association with hard X-ray 'microflares' and chromospheric evaporation may make them extremely important in the energetics of active regions and in the maintenance of their enhanced coronal emission. Title: Spectral Line Profiles of Fe XXI 1354.1 Angstrom from the Solar Maximum Mission Authors: Mason, H. E.; Shine, R. A.; Gurman, J. B.; Harrison, R. A. Bibcode: 1986ApJ...309..435M Altcode: Observations of the Fe XXI 1354.1 A line were obtained for several flares using the SMM-UVSP instrument with varying spectral and spatial resolution. Of special interest are spectral line profiles from the footpoints of flare loops taken during the impulsive phase. These data show blueshifted Fe XXI profiles coincident and cospatial with the impulsive brightening of chromospheric material. The present analysis supports the hypothesis that the blueshifted component of the high temperature emission is an integral part of the flare, possibly associated with chromospheric evaporation. Title: SMM Observations of Non-Linear Oscillations in the C IV 1548Å Line above a Sunspot Authors: Shine, R. A.; McWhirter, R. W. P. Bibcode: 1986BAAS...18Q.990S Altcode: No abstract at ADS Title: White Light Observations of a Sunspot Penumbra and its Interaction with the Surrounding Photosphere Authors: Shine, R. A.; SOUP Team Bibcode: 1986BAAS...18..661S Altcode: No abstract at ADS Title: Second Generation Spectrograph for the Hubble Space Telescope Authors: Maran, S. P.; Woodgate, B. E.; Boggess, A.; Gull, T. R.; Heap, S. R.; Melcher, R.; Green, R. F.; Wolff, S. C.; Hutchings, J. B.; Jenkins, E. B.; Linsky, J. L.; Moos, H. W.; Roesler, F.; Shine, R. A.; Timothy, J. G.; Weistrop, D. E. Bibcode: 1986BAAS...18..636M Altcode: No abstract at ADS Title: Chromospheric explosions. Authors: Doschek, G. A.; Antiochos, S. K.; Antonucci, E.; Cheng, C. -C.; Culhane, J. L.; Fisher, G. H.; Jordan, C.; Leibacher, J. W.; MacNiece, P.; McWhirter, R. W. P.; Moore, R. L.; Rabin, D. M.; Rust, D. M.; Shine, R. A. Bibcode: 1986NASCP2439....4D Altcode: The work of this team addressed the question of the response and relationship of the flare chromosphere and transition region to the hot coronal loops that reach temperatures of about 107K and higher. Flare related phenomena such as surges and sprays are also discussed. The team members debated three main topics: 1. whether the blue-shifted components of X-ray spectral lines are signatures of "chromospheric evaporation"; 2. whether the excess line broadening of UV and X-ray lines is accounted for by "convective velocity distribution" in evaporation; and 3. whether most chromospheric heating is driven by electron beams. Title: Second generation spectrograph for the Hubble Space Telescope. Authors: Woodgate, B. E.; Boggess, A.; Gull, T. R.; Heap, S. R.; Krueger, V. L.; Maran, S. P.; Melcher, R. W.; Rebar, F. J.; Vitagliano, H. D.; Green, R. F.; Wolff, S. C.; Hutchings, J. B.; Jenkins, E. B.; Linsky, J. L.; Moos, H. W.; Roesler, F.; Shine, R. A.; Timothy, J. G.; Weistrop, D. E.; Bottema, M.; Meyer, W. Bibcode: 1986SPIE..627..350W Altcode: The preliminary design for the Space Telescope Imaging Spectrograph (STIS), which has been selected by NASA for definition study for future flight as a second-generation instrument on the Hubble Space Telescope (HST), is presented. STIS is a two-dimensional spectrograph that will operate from 1050 A to 11,000 A at the limiting HST resolution of 0.05 arcsec FWHM, with spectral resolutions of 100, 1200, 20,000, and 100,000 and a maximum field-of-view of 50 x 50 arcsec. Its basic operating modes include echelle model, long slit mode, slitless spectrograph mode, coronographic spectroscopy, photon time-tagging, and direct imaging. Research objectives are active galactic nuclei, the intergalactic medium, global properties of galaxies, the origin of stellar systems, stelalr spectral variability, and spectrographic mapping of solar system processes. Title: White-light movies of the solar photosphere from the soup instrument on spacelab 2 Authors: Title, A. M.; Tarbell, T. D.; Simon, G. W.; Acton, L.; Duncan, D.; Ferguson, S.; Finch, M.; Frank, Z.; Kelly, G.; Lindgren, R.; Morrill, M.; Pope, T.; Reeves, R.; Rehse, R.; Shine, R.; Topka, K.; Harvey, J.; Leibacher, J.; Livingston, W.; November, L. Bibcode: 1986AdSpR...6h.253T Altcode: 1986AdSpR...6..253T We present initial results on solar granulation, pores and sunspots from the white-light films obtained by the Solar Optical Universal Polarimeter (SOUP) instrument on Spacelab 2. SOUP contains a 30-cm Cassegrain telescope, an active secondary mirror for image stabilization, and a white-light optical system with 35-mm film and video cameras. Outputs from the fine guidance servo provided engineering data on the performance of the ESA Instrument Pointing System (IPS). Several hours of movies were taken at various disk and limb positions in quiet and active regions. The images are diffraction-limited at 0.5 arc second resolution and are, of course, free of atmospheric seeing and distortion. Properties of the granulation in magnetic and non-magnetic regions are compared and are found to differ significantly in size, rate of intensity variation, and lifetime. In quiet sun on the order of fifty percent of the area has at least one ``exploding granule'' occurring in it during a 25 minute period. Local correlation tracking has detected several types of transverse flows, including systematic outflow from the penumbral boundary of a spot, motion of penumbral filaments, and cellular flow patterns of supergranular and mesogranular size. Feature tracking has shown that in quiet sun the average granule fragment has a velocity of about one kilometer per second. Title: Multiwavelength Analysis of a Well Observed Flare from Solar Maximum Mission Authors: MacNeice, P.; Pallavicini, R.; Mason, H. E.; Simnett, G. M.; Antonucci, E.; Shine, R. A.; Rust, D. M.; Jordan, C.; Dennis, B. R. Bibcode: 1985SoPh...99..167M Altcode: We describe and analyse observations of an M1.4 flare which began at 17: 00 UT on 12 November, 1980. Ground based Hα and magnetogram data have been combined with EUV, soft and hard X-ray observations made with instruments on-board the Solar Maximum Mission (SMM) satellite. The preflare phase was marked by a gradual brightening of the flare site in Ov and the disappearance of an Hα filament. Filament ejecta were seen in Ov moving southward at a speed of about 60 km s−1, before the impulsive phase. The flare loop footpoints brightened in Hα and the CaXIX resonance line broadened dramatically 2 min before the impulsive phase. Non-thermal hard X-ray emission was detected from the loop footpoints during the impulsive phase while during the same period blue-shifts corresponding to upflows of 200-250 km s−1 were seen in Ca XIX. Evidence was found for energy deposition in both the chromosphere and corona at a number of stages during the flare. We consider two widely studied mechanisms for the production of the high temperature soft X-ray flare plasma in the corona, i.e. chromospheric evaporation, and a model in which the heating and transfer of material occurs between flux tubes during reconnection. Title: Association of Small, Bright Photospheric Features with Magnetic Fields Authors: Topka, K.; Shine, R.; SOUP Team Bibcode: 1985BAAS...17..834T Altcode: No abstract at ADS Title: Erratum - a Study of Flare Buildup from Simultaneous Observations in Microwave Hα and Ultraviolet Wavelengths Authors: Kundu, M. R.; Gaizauskas, V.; Woodgate, B. E.; Schmahl, E. J.; Shine, R.; Jones, H. P. Bibcode: 1985ApJS...58..195K Altcode: No abstract at ADS Title: A study of flare buildup from simultaneous observations in microwave, H-alpha, and UV wavelengths Authors: Kundu, M. R.; Gaizauskas, V.; Woodgate, B. E.; Schmahl, E. J.; Shine, R.; Jones, H. P. Bibcode: 1985ApJS...57..621K Altcode: The results of high-resolution observations of the solar preflare activity of June 25, 1980 are analyzed. The observations were carried out simultaneously in the UV microwave, and H-alpha wavelengths using the VLA, the Ottawa River photoheliograph, and the Solar Max spectrometer and polarimeter instruments. Increases were observed in the intensitiy and polarization of compact sources at a wavelength of 6-cm during the preflare hour. The increases were associated with rising and twisting motions in the magnetic loops near the sight of the subsequent flare. Consistent with this process, analysis of the transverse and Doppler motions observed in the H-alpha filament before disruption showed that the filament was activated internally by the motions of evolving magnetic flux patterns. Ultraviolet data for C IV brightenings and upflows at the first appearance of the H-alpha filament indicated the presence of rising magnetic loops and material rising within the loops. The complete VLA, microwave and H-alpha data sets are given. Title: Absolute Wavelength Measurements of Solar UV Emission Lines Authors: Bruner, M. E.; Shine, R. A. Bibcode: 1985BAAS...17..630B Altcode: No abstract at ADS Title: Energy Release and Energy Transport Below the Transition Zone in Solar Flares Authors: Hénoux, J. C.; Chambe, G.; Heristchi, D.; Semel, M.; Woodgate, B.; Shine, R.; Beckers, J. Bibcode: 1985spit.conf..758H Altcode: No abstract at ADS Title: Center-to-Limb Variation of Transition Region Redshift Authors: Shine, R. A.; Woodgate, B. E.; Gurman, J. B. Bibcode: 1984BAAS...16..992S Altcode: No abstract at ADS Title: Evidence for Chromospheric Evaporation in Solar Flares from UV Observations Authors: Shine, R. A.; Mason, H. E. Bibcode: 1984BAAS...16..543S Altcode: No abstract at ADS Title: Scientific Results from the Ultraviolet Spectrometer and Polarimeter on SMM Authors: Shine, R. A. Bibcode: 1984stp..conf...91S Altcode: No abstract at ADS Title: Optical, microwave and UV imagery of a solar flare. Authors: Gaizauskas, V.; Kundu, M. R.; Schmahl, E. J.; Shine, R. A.; Woodgate, B. E. Bibcode: 1983JRASC..77..261G Altcode: No abstract at ADS Title: Formation of the CL I line at 1351 A in the solar chromosphere Authors: Shine, R. A. Bibcode: 1983ApJ...266..882S Altcode: The formation of the multiplet containing the Cl I 1351 A line is investigated due to the unusual brightness of this line. It is determined that this line is formed via a fluorescence effect driven by the 1335 A line of C II. Non-LTE calculations including this effect are found to agree with the observed line intensity. It is shown that the 1347 and 1363 A lines of Cl I do not benefit from this effect and they are predicted to be approximately 100 times weaker. Title: Conductive flux in flaring solar chromospheres deduced from the linear polarization observations Authors: Henoux, J. C.; Heristchi, D.; Chambe, G.; Woodgate, B.; Shine, R.; Beckers, J.; Machado, M. Bibcode: 1983A&A...119..233H Altcode: The linear polarization of Hα and S I 1437 Å lines produced in impact excitation by energetic electrons with an anisotropic velocity distribution function during solar flares is calculated. Selecting a function which represents the velocity distribution of electrons carrying heat flux, the relationship between conductive heat flux and linear line polarization has been computed.

The application of the relationship between linear polarization and heat flux to the observed degree of polarization leads to the determination of the conductive heat flux at the top of flaring chromospheric layers. This conductive flux is of the order of magnitude of the total radiation loss in the chromosphere and below, which is also of the order of magnitude of the conductive flux in the transition zone. Title: Simultaneous ultraviolet line and hard X-ray bursts in the impulsive phase of solar flares Authors: Woodgate, B. E.; Shine, R. A.; Poland, A. I.; Orwig, L. E. Bibcode: 1983ApJ...265..530W Altcode: Several fast impulsive phase solar flare bursts were observed by the Solar Maximum Mission instruments on 1980 November 8. The bursts were seen to be coincident in the O V 1371 Å line formed at 2.5 × 105 K and in 25-300 keV X-rays, to within the resolution time of 1 s. This lack of time difference is inconsistent with models for these flares in which the hard X-rays are produced at the top of a loop, followed by the formation of a thermal conduction front which travels to the footpoint where a UV burst is produced by heating. Models in which both X-rays and UV radiation are produced at the footpoint, or an electron beam transmits energy between loop top and footpoint is less than 1 s, are allowed. Title: Fluid motions in the solar chromosphere-corona transition region. I - Line widths and Doppler shifts for C IV Authors: Athay, R. G.; Gurman, J. B.; Henze, W.; Shine, R. A. Bibcode: 1983ApJ...265..519A Altcode: Matrices of line profiles for C IV, λ1548, observed with a 3" aperture and sampled in 3" intervals in active and quiet solar regions, show a pronounced tendency for line width to increase with increasing redshift. The correlation between increasing central intensity of the line and increasing redshift demonstrated by some authors is clearly present in these data but is weakened by the not infrequent occurrence of regions of strong redshift but with low intensity. Sunspots show both systematically narrower line profiles over umbral areas and strong redshifts on their Sun-center side. The latter result is consistent with a reverse Evershed effect. Title: Observations of the Longitudinal Magnetic Field in the Transition Region and Photosphere of a Sunspot Authors: Henze, W., Jr.; Tandberg-Hanssen, E.; Hagyard, M. J.; West, E. A.; Woodgate, B. E.; Shine, R. A.; Beckers, J. M.; Bruner, M.; Hyder, C. L.; West, E. A. Bibcode: 1982SoPh...81..231H Altcode: The Ultraviolet Spectrometer and Polarimeter on the Solar Maximum Mission spacecraft has observed for the first time the longitudinal component of the magnetic field by means of the Zeeman effect in the transition region above a sunspot. The data presented here were obtained on three days in one sunspot, have spatial resolutions of 10 arc sec and 3 arc sec, and yield maximum field strengths greater than 1000 G above the umbrae in the spot. The method of analysis, including a line-width calibration feature used during some of the observations, is described in some detail in an appendix; the line width is required for the determination of the longitudinal magnetic field from the observed circular polarization. Title: Measurements of solar transition zone velocities and line broadening using the ultraviolet spectrometer and polarimeter on the Solar Maximum Mission Authors: Simon, G.; Mein, P.; Vial, J. C.; Shine, R. A.; Woodgate, B. E. Bibcode: 1982A&A...115..367S Altcode: The UVSP instrument on SMM is able to observe solar regions at two wavelengths in the same line with a band-pass of 0.3 A. Intensity and Doppler velocity maps are derived. It is shown that the numerical values are sensitive to the adopted Doppler width and the range of velocities is limited to within 30 km/sec. A method called Double Dopplergram Determination (DDD) is described for deriving both the Doppler width and the velocity (up to 80 km/sec), and the main sources of uncertainties are discussed. To illustrate the method, a set of C IV 1548 A observations is analyzed according to this procedure. The mean C IV Doppler width measured (0.15 A) is comparable to previous determinations. A relation is found between bright regions and down-flows. Large Doppler widths correspond to strong velocity gradients. Title: Fluid motions the solar chromosphere-corona transition region. II Active region flows in C IV from narrow slit Dopplergrams Authors: Athay, R. G.; Gurman, J. B.; Shine, R. A.; Henze, W. Bibcode: 1982ApJ...261..684A Altcode: From a study of Dopplergrams made with two narrow slits in the opposite wings of the C IV line, N λ1548, we find widespread evidence for steady flow patterns associated with large sunspots and, on a larger scale, with active region magnetic field patterns. The characteristic sunspot flow is in the reverse Evershed sense with a substantial vertical component. Active region flows indicate oppositely directed velocities with mainly horizontal components on either side of magnetic neutral lines. Some neutral lines show flow toward the neutral line, whereas others show flow away from the neutral line. Title: Relation of Ephemeral Magnetic Regions to the Low Amplitude Branch of Persistent Vertical Velocities Authors: Gebbie, K. B.; Toomre, J.; Haber, D. A.; Hill, F.; Simon, G. W.; November, L. J.; Gurman, J. B.; Shine, R. A. Bibcode: 1982BAAS...14R.939G Altcode: 1982BAAS...14..939G No abstract at ADS Title: Upflows Immediately Prior to the Impulsive Phase of Solar Flares Authors: Woodgate, B. E.; Shine, R. A.; Schmahl, E. J.; Kundu, M.; Gaizauskas, V. Bibcode: 1982BAAS...14..898W Altcode: No abstract at ADS Title: Formation of the O I resonance triplet and intercombination doublet in the solar chromosphere Authors: Skelton, D. L.; Shine, R. A. Bibcode: 1982ApJ...259..869S Altcode: Spectrum synthesis calculations are presented for the O I resonance triplet at 1304 A and the intercombination doublet at 1358 A for the solar atmosphere and several variants, allowing for triplet fluorescence by the Ly-beta emission of H I. Profiles, synthesized from a seven-level plus continuum O I atom are compared to observations taken with the high-resolution spectrometer on OSO 8. It is found that the O I triplet emission is dominated by the Ly-beta fluorescence and that the agreement between observations and profiles computed with current chromospheric models is much improved over earlier studies. Title: Mass motions in the solar chromosphere and transition zone Authors: Mein, P.; Simon, G.; Vial, J. C.; Shine, R. A. Bibcode: 1982A&A...111..136M Altcode: A comparison is made between H-alpha and C IV observations of Active Region 2717 on October 9, 1980. On the basis of this comparison, it is found that upward velocities are present above sunspots in the chromosphere-corona transition zone (20 km/s). The downward velocities are found to be well correlated in both lines. Doppler-shift ratios between C IV and H-alpha levels (approximately 10) are seen to be much smaller than expected from density ratio estimates. The comparison is seen as suggesting that flow lines are probably far from vertical in the transition zone. It is pointed out, however, that this depends on model densities that may not be correct. A simple method for comparing matter flows is presented. The best fit between H-alpha and C IV levels is obtained when C IV Doppler shifts are multiplied by the line intensity to the power 0.5 (approximately) in order to make allowance for density fluctuations. Title: The Impulsive and Gradual Phases of a Solar Limb Flare as Observed from the Solar Maximum Mission Satellite Authors: Poland, A. I.; Machado, M. E.; Wolfson, C. J.; Frost, K. J.; Woodgate, B. E.; Shine, R. A.; Kenny, P. J.; Cheng, C. C.; Tandberg-Hanssen, E. A.; Bruner, E. C.; Henze, W. Bibcode: 1982SoPh...78..201P Altcode: Simultaneous observations of a solar limb flare in the X-ray and ultraviolet regions of the spectrum are presented. Temporal and spectral X-ray observations were obtained for the 25-300 keV range while temporal, spectral, and spatial X-ray observations were obtained for the 30-0.3 keV range. The ultraviolet observations were images with a 10″ spatial resolution in the lines of O v (Te ∼ 2.5 × 105 K) and Fe XXI (Te ∼ 1.1 × 107 K). The hard X-ray and O v data indicate that the impulsive phase began in the photosphere or chromosphere and continued for several minutes as material was ejected into the corona. Impulsive excitation was observed up to 30 000 km above the solar surface at specific points in the flare loop. The Fe XXI observations indicate a preheating before the impulsive phase and showed the formation of hot post-flare loops. This later formation was confirmed by soft X-ray observations. These observations provide limitations for current flare models and will provide the data needed for initial conditions in modeling the concurrent coronal transient. Title: Evidence of redshifts in the average solar line profiles of C iv and Si iv from OSO-8 observations Authors: Roussel-Dupre, D.; Shine, R. A. Bibcode: 1982SoPh...77..329R Altcode: Measurements of the C IV 1548 Å and Si IV 1393 Å lines made with the University of Colorado Ultraviolet Spectrometer on board OSO-8 show that the mean profiles are redshifted at disk center. Assuming these lines to be optically thin, we measure an apparent average downflow of material in the 50 000 to 100 000 K temperature range which is weighted by the emission measure in these lines. The magnitude of the redshift varies from 6-17 km s−1 with a mean of 12 km s−1 and is persistent at least on the order of months, which is the time covered by the observations presented in this paper. Pneuman and Kopp (1978) have demonstrated that the flux of material associated with this downflow is of the same order of magnitude as the flux of material being carried upward in spicules. Thus, it is possible that material observed to be downflowing in C IV and Si IV has its origins in the upward moving spicule material. Title: Transition region oscillations in sunspots. Authors: Gurman, J. B.; Leibacher, J. W.; Shine, R. A.; Woodgate, B. E.; Henze, W. Bibcode: 1982ApJ...253..939G Altcode: Time series observations of the profile of the C IV resonance line 1548.19 A obtained in eight sunspots with the Ultraviolet Spectrometer and Polarimeter (UVSP) on the Solar Maximum Mission are discussed. All of the sunspots exhibit significant oscillations in line-of-sight velocity with frequencies in the range from 5.8 mHz to 7.8 mHz (periods of 129-173 s). Significant intensity oscillations are observed at the same periods in four of the time series; the maximum intensity is in phase with maximum blueshift. Difference spectroheliograms ('Dopplergrams') of the two halves of the C IV line, as well as observations in the Si IV resonance line 1402.77 A and the O IV intersystem line 1401.16 A, also reveal velocity oscillations at similar frequencies but only over sunspots. Title: Observations of solar flare transition zone plasmas from the Solar Maximum Mission Authors: Cheng, C. -C.; Bruner, E. C.; Tandberg-Hanssen, E.; Woodgate, B. E.; Shine, R. A.; Kenny, P. J.; Henze, W.; Poletto, G. Bibcode: 1982ApJ...253..353C Altcode: The spatial and temporal evolution of the Si IV and O IV intensity, density and mass motions in preflare and flare transition zone plasmas are studied for the case of the April 8, 1980 flare. It is found that: (1) the UV flare observed in the Si IV and O IV lines is unambiguously identified as occurring in a low-lying, preexisting transition zone loop which spanned the magnetic neutral line separating a larger leader spot and a newly emerged, isolated spot of opposite polarity; (2) at the onset of the flare, the easternmost footpoint, which was anchored in an isolated spot region of high longitudinal magnetic field gradient, showed sudden, impulsive brightening with large intensity increases; and (3) the release flare energy was transported by way of large-scale connecting field lines to other parts of the active region, producing the hot plasma and H-alpha kernels observed near the trailing spot. Title: Impact linear polarization observed in a UV chromospheric line during a solar flare Authors: Henoux, J. C.; Chambe, G.; Semel, M.; Woodgate, B.; Shine, R.; Beckers, J. Bibcode: 1982AdSpR...2k.155H Altcode: 1982AdSpR...2..155H Linear polarization was observed in the S I 1437Å line in bright flaring points during the soft X-ray emission. The degree of polarization is about 25% and is detected at a signal to noise ratio of 2.9. The polarized electric vector is directed towards disk center to within 3°.

This polarization could be due to collisional excitationm of S I by energetic electrons beamed in the vertical direction. We suggest that the heat flux in the region interconnecting the transition zone to the high chromosphere during the gradual phase of a flare could lead to an anisotropic excitation. Then the observed polarization would be due to vertical motions of the transition zone sweeping the preexisting chromosphere. Title: Steady flows in the solar transition region observed with SMM Authors: Gebbie, K. B.; Hill, F.; November, L. J.; Gurman, J. B.; Shine, R. A.; Woodgate, B. E.; Athay, R. G.; Tandberg-Hanssen, E. A.; Toomre, J.; Simon, G. W. Bibcode: 1981ApJ...251L.115G Altcode: Steady flows in the quiet solar transition region have been observed with the Ultraviolet Spectrometer and Polarimeter experiment on the Solar Maximum Mission (SMM) satellite. The persistent vertical motions seen at disk center have spatial rms amplitudes of 1.4 km/s in the C II line, 3.9 km/s in Si IV, and 4.2 km/s in C IV. The amplitudes of the more horizontal flows seen toward the limb tend to be somewhat higher. Plots of steady vertical velocity versus intensity seen at disk center in Si IV and C IV show two distinct branches. Title: Spatial and temporal structures of impulsive bursts from solar flares observed in UV and hard X-rays Authors: Cheng, C. -C.; Tandberg-Hanssen, E.; Bruner, E. C.; Orwig, L.; Frost, K. J.; Kenny, P. J.; Woodgate, B. E.; Shine, R. A. Bibcode: 1981ApJ...248L..39C Altcode: New observations are presented of impulsive UV and hard X-rays bursts in two solar flares obtained with instruments on Solar Maximum Mission. The UV bursts were observed in the Si IV and O IV emission lines, whose intensity ratio is density-sensitive. By comparing the spatially resolved Si IV/O IV observations with the corresponding hard X-ray observations, it is possible to study their spatial and temporal relationships. For one flare, the individual component spikes in the multiply peaked hard X-ray burst can be identified with different discrete Si IV/O IV flaring kernels of size 4 arcsec x 4 arcsec or smaller, which brighten up sequentially in time. For the other, many Si IV/O kernels, widely distributed over a large area, show impulsive bursts at the same time, which correlate with the main peak of the impulsive hard X-ray burst. The density of the flaring Si IV/O IV kernels is in the range from 5 x 10 to the 12th-13th/cu cm. Title: Excitation of the Chlorine I Line at 1351Å Authors: Shine, R. A.; Woodgate, B. E.; Ayres, T. R. Bibcode: 1981BAAS...13Q.830S Altcode: No abstract at ADS Title: Flare Buildup at 6 cm Wavelength, in UV and Hα Authors: Schmahl, E. J.; Kundu, M. R.; Woodgate, B.; Shine, R. Bibcode: 1981BAAS...13..846S Altcode: No abstract at ADS Title: Observations of the 1980 April 30 limb flare by the ultraviolet spectrometer and polarimeter on the Solar Maximum Mission Authors: Woodgate, B. E.; Shine, R. A.; Brandt, J. C.; Chapman, R. D.; Michalitsianos, A. G.; Kenny, P. J.; Bruner, E. C.; Rehse, R. A.; Schoolman, S. A.; Cheng, C. C. Bibcode: 1981ApJ...244L.133W Altcode: Observations of the M2 limb flare of 1980 April 30 by the ultraviolet spectrometer and polarimeter in the C IV 1548 A line are described and compared with observations from other SMM instruments and with ground-based H-alpha data. Events observed during the 18 minutes leading up to the flare impulsive phase include the filling of a small loop with material moving at about 20 km/s, followed by a rapid brightening in C IV, H-alpha, and hard X-rays, with a subsequent brightening of a higher set of loops. The rapid brightening appears to be at the junction of the small loop with the overlying magnetic structures, which suggests the flare may be caused by their interaction. Title: SMM/UVSP Observations of Oscillations and Other Properties in a Sunspot Authors: Henze, W.; Tandberg-Hanssen, E.; Reichmann, E. J.; Shine, R. A.; Woodgate, B. E.; Gurman, J. B.; Athay, R. G. Bibcode: 1981BAAS...13..858H Altcode: No abstract at ADS Title: Height Dependence of Steady Flows Determined from Coordinated SMM and SPO Observations Authors: Gebbie, K. B.; Hill, F.; Toomre, J.; November, L. J.; Simon, G. W.; Gurman, J. B.; Shine, R. A.; Woodgate, B. E. Bibcode: 1981BAAS...13..914G Altcode: No abstract at ADS Title: Solar maximum mission experiment: Ultraviolet spectroscopy and polarimetry on the solar maximum mission Authors: Tandberg-Hanssen, E.; Cheng, C. C.; Woodgate, B. E.; Brandt, J. C.; Chapman, R. D.; Kenney, P. J.; Michalitsianos, A. G.; Shine, R. A.; Athay, R. G.; Beckers, J. M.; Bruner, E. C.; Rehse, R. A.; Schoolman, S. A.; Gurman, J. B.; Hyder, C. L.; Henze, W. Bibcode: 1981AdSpR...1m.275T Altcode: 1981AdSpR...1..275T We describe the Ultraviolet Spectrometer and Polarimeter (UVSP) on the Solar Maximum Mission (SMM) spacecraft. The instrument, which operates in the wavelength range 1150 - 3600 Å, has a spatial resolution of 2-3 arc sec and a spectral resolution of 0.02 Å FWHM in second order. A Gregorian telescope, focal length 1.8 m, feeds a 1 m Ebert-Fastie spectrometer. A polarimeter comprising rotating Mg F2 waveplates can be inserted behind the spectrometer entrance slit and allows all four Stokes parameters to be determined. The observing modes include rasters, spectral scans, velocity measurements, and polarimetry. Finally, we present examples of initial observations made since launch. Title: Solar Maximum Mission experiment: ultraviolet spectroscopy and polarimetry on the Solar Maximum Mission. Authors: Tandberg-Hanssen, E.; Woodgate, B. E.; Athay, R. G.; Beckers, J. M.; Brandt, J. C.; Bruner, E. C.; Chapman, R. D.; Cheng, C. -C.; Gurman, J. B.; Hyder, C. L.; Kenney, P. J.; Michalitsianos, A. G.; Rehse, R. A.; Schoolman, S. A.; Shine, R. A.; Henze, W. Bibcode: 1981hea..conf..275T Altcode: No abstract at ADS Title: UVSP/SMM observations of transition region oscillations in sunspots Authors: Gurman, J. B.; Shine, R. A.; Woodgate, B. E.; Leibacher, J. W.; Henze, W. Bibcode: 1981phss.conf..319G Altcode: Using Ultraviolet Spectrometer and Polarimeter data obtained in emission lines formed at temperatures of 70,000 K to 130,000 K, transition region oscillations in sunspots have been observed. The frequency of these oscillations lies in the range 5.8 mHz to 7.8 mHz. Their regular appearance in line-of-sight velocity and their frequent occurrence in intensity in phase with maximum blue shift leads to the interpretation of the oscillations as upward-propagating acoustic waves. The presence in two of the C IV wavelength 1548.19 time series of a phase-shifted oscillation in the line width may be caused by the presence of unidentified blends in the line wings. The energy flux carried by the umbral acoustic waves is less than 2000 erg/sq cm/s, some seven orders of magnitude smaller than the missing radiative flux of sunspots. Title: The photospheric vector magnetic field of a sunspot and its vertical gradient Authors: Hagyard, M. J.; West, E. A.; Tandberg-Hanssen, E.; Smith, J. E.; Henze, W., Jr.; Beckers, J. M.; Bruner, E. C.; Hyder, C. L.; Gurman, J. B.; Shine, R. A. Bibcode: 1981phss.conf..213H Altcode: The results of direct comparisons of photospheric and transition region line-of-sight field observations of sunspots using the SMM UV spectrometer and polarimeter are reported. The analysis accompanying the data is concentrated on demonstrating that the sunspot concentrated magnetic field extends into the transition region. An observation of a sunspot on Oct. 23, 1980 at the S 18 E 03 location is used as an example. Maximum field strengths ranged from 2030-2240 gauss for large and small umbrae viewed and inclination of the field to the line-of-sight was determined for the photosphere and transition region. The distribution of the magnetic field over the sunspot and variation of the line-of-sight gradient are discussed, as are the magnitudes and gradients of the photospheric field across the penumbral-photospheric boundaries. Title: The Development of Flares Observed in the Spectral Lines OV 1371 Å, FeXXI 1354 Å, and in Hard X-Rays Authors: Woodgate, B. E.; Bruner, E. C.; Cheng, C. C.; Dennis, B. R.; Gurman, J. B.; Frost, K. J.; Hyder, C. L.; Kiplinger, A.; Mason, H. E.; Orwig, L. E.; Poland, A. I.; Schoolman, S. A.; Shine, R. A.; Tandberg-Hanssen, E. A. Bibcode: 1980BAAS...12..911W Altcode: No abstract at ADS Title: Steady Flows in the Solar Transition Region Observed with the UVSP Experiment on SMM Authors: Gebbie, K. B.; Hill, F.; Toomre, J.; November, L. J.; Simon, G. W.; Athay, R. G.; Bruner, E. C.; Rehse, R.; Gurman, J. B.; Shine, R. A.; Woodgate, B. E.; Tandberg-Hanssen, E. A. Bibcode: 1980BAAS...12..907G Altcode: No abstract at ADS Title: Transition Region Oscillations in Sunspots Authors: Gurman, J. B.; Shine, R. A.; Woodgate, B. E.; Tandberg-Hanssen, E. A.; Bruner, E. C.; Schoolman, S. A.; Athay, R. G. Bibcode: 1980BAAS...12..906G Altcode: No abstract at ADS Title: The Spatial Dependence of UV and X-Ray Phenomena Occurring During the Impulsive Phase of a Flare Authors: Frost, K. J.; Dennis, B. R.; Orwig, L. E.; Kiplinger, A. L.; Leibacher, J.; Antonucci, E.; Parmar, A. N.; Woodgate, B.; Shine, R.; Cheng, C. -C. Bibcode: 1980BAAS...12..905F Altcode: No abstract at ADS Title: SMM/UVSP Observations of Magnetic Fields in the Transition Region above Sunspots Authors: Henze, W.; Beckers, J. M.; Gurman, J. B.; Hyder, C. L.; Schoolman, S. A.; Shine, R. A.; Tandberghanssen, E.; Woodgate, B. E.; Hagyard, M. J. Bibcode: 1980BAAS...12R.896H Altcode: No abstract at ADS Title: Correlations Between UV and X-Rays for the June 29, 1980 Flare at 02:34 Authors: Shine, R. A.; Woodgate, B. E.; Dennis, B. R.; Cheng, C. C.; Wolfson, J.; Bruner, E. C.; Hyder, C. L. Bibcode: 1980BAAS...12Q.903S Altcode: No abstract at ADS Title: UV Observations of the June 29, 1980 Flare at 18:24UT Authors: Poland, A. I.; Woodgate, B. E.; Shine, R. A.; Frost, K. J.; Kenny, P.; Bruner, E. C.; Wolfson, J.; Cheng, C. C.; Tandberg-Hanssen, E. A.; Gurman, J.; Henze, W.; Machado, M. Bibcode: 1980BAAS...12..903P Altcode: No abstract at ADS Title: Sunspot Observations with the Ultraviolet Spectrometer and Polarimeter Experiment on the Solar Maximum Mission Authors: Gurman, J. B.; Woodgate, B. E.; Shine, R. A.; Brandt, J. C.; Chapman, R. D.; Michalitsianos, A. G.; Kenny, P. J.; Bruner, E. C.; Rehse, R.; Schoolman, S. A.; Cheng, C. C.; Tandberg-Hanssen, E. A.; Athay, G. R.; Beckers, J. M.; Henze, W.; Brown, Teledyne; Hyder, C. L. Bibcode: 1980BAAS...12..535G Altcode: No abstract at ADS Title: Density Diagnostic of Solar Active Region and Flare Plasmas from Si IV/O IV Line Ratio as Observed from SMM Authors: Bruner, E. C.; Rehse, R.; Schoolman, S. A.; Brandt, J. C.; Chapman, R. D.; Kenny, P. J.; Michalitsianos, A. G.; Shine, R. A.; Woodgate, B. E.; Cheng, C. C.; Tandberg-Hanssen, E. A.; Athay, G. R.; Beckers, J. M.; Gurman, J.; Henze, W.; Brown, Teledyne; Hyder, C. L. Bibcode: 1980BAAS...12R.539B Altcode: No abstract at ADS Title: Density diagnostic of solar active region and flare plasmas from Si IV/O IV line ratio as observed from SMM (Solar Maximum Mission). Authors: Bruner, E. C.; Rehse, R.; Schoolman, S. A.; Brandt, J. C.; Chapman, R. D.; Kenny, P. J.; Michalitsianos, A. G.; Shine, R. A.; Woodgate, B. E.; Cheng, C. -C.; Tandberg-Hanssen, E. A.; Athay, G. R.; Beckers, J. M.; Gurman, J. B.; Henze, W.; Hyder, C. L. Bibcode: 1980BAAS...12..534B Altcode: No abstract at ADS Title: Solar Flare and Surge Image Sequences as Seen by the Ultraviolet Spectrometer and Polarimeter on SMM Authors: Henze, W.; Brown, Teledyne; Brandt, J. C.; Chapman, R. D.; Kenny, P. J.; Michalitsianos, A. G.; Shine, R. A.; Woodgate, B. E.; Bruner, E. C.; Rehse, R.; Schoolman, S. A.; Cheng, C. C.; Tandberg-Hanssen, E. A.; Athay, G. R.; Beckers, J. M.; Gurman, J.; Hyder, C. L. Bibcode: 1980BAAS...12..532H Altcode: No abstract at ADS Title: The Ultraviolet Spectrometer and Polarimeter (UVSP) on the Solar Maximum Mission and Initial Results in Polarimetry Authors: Tandberg-Hanssen, E.; Athay, R. G.; Bruner, E. C.; Beckers, J. M.; Brandt, J. C.; Chapman, R. D.; Cheng, C. C.; Gurman, J.; Henze, W.; Brown, Teledyne; Hyder, C. L.; Michalitsianos, A. G.; Shine, R. A.; Schoolman, S. A.; Woodgate, B. E. Bibcode: 1980BAAS...12..534T Altcode: No abstract at ADS Title: The Dynamics of Solar Flares and Surges as Seen at the Solar Limb in the Transition Zone Authors: Woodgate, B. E.; Brandt, J. C.; Chapman, R. D.; Kenny, P. J.; Michalitsianos, A. G.; Shine, R. A.; Bruner, E. C.; Rehse, R.; Schoolman, S. A.; Cheng, C. C.; Tandbert-Hanssen, E. A.; Athay, G. R.; Beckers, J. M.; Gurman, J.; Henze, W.; Brown, Teledyne; Hyder, C. L. Bibcode: 1980BAAS...12Q.535W Altcode: No abstract at ADS Title: Active Region Morphology and Evolution Images from the Ultraviolet Spectrometer and Polarimeter Authors: Shine, R. A.; Brandt, J. C.; Chapman, R. D.; Kenny, P. J.; Michalitsianos, A. G.; Woodgate, B. E.; Bruner, E. C.; Rehse, R.; Schoolman, S. A.; Cheng, C. C.; Tandberg-Hanssen, E. A.; Athay, G. R.; Beckers, J. M.; Gurman, J.; Henze, W.; Brown, Teledyne; Hyder, C. L. Bibcode: 1980BAAS...12R.531S Altcode: No abstract at ADS Title: Line formation in the solar chromosphere. II - an optically thick region of the chromosphere-corona transition region observed with OSO 8 Authors: Lites, B. W.; Hansen, E. R.; Shine, R. A. Bibcode: 1980ApJ...236..280L Altcode: The University of Colorado ultraviolet spectrometer aboard the Orbiting Solar Observatory 8(OSO 8) has measured self-reversed profiles of the resonance line of C IV lamda 1548.2 at the limb passage of an active region. The degree of the self-reversal together with the absolute intensity of the line profile determine the electron density in the active region at 10 to the 10th/cu cm at temperatures where the C IV line is formed. The nonthermal component of the broadening velocity is no more than 14km/s, and the physical thickness of an equivalent plane-parallel slab in hydrostatic equilibrium that would give rise to the observed line profiles is about 430 km. Title: The ultraviolet spectrometer and polarimeter on the Solar Maximum Mission. Authors: Woodgate, B. E.; Tandberg-Hanssen, E. A.; Bruner, E. C.; Beckers, J. M.; Brandt, J. C.; Henze, W.; Hyder, C. L.; Kalet, M. W.; Kenny, P. J.; Knox, E. D.; Michalitsianos, A. G.; Rehse, R.; Shine, R. A.; Tinsley, H. D. Bibcode: 1980SoPh...65...73W Altcode: The Ultraviolet Spectrometer and Polarimeter (UVSP) on the Solar Maximum Mission spacecraft is described, including the experiment objectives, system design, performance, and modes of operation. The instrument operates in the wavelength range 1150-3600 Å with better than 2 arc sec spatial resolution, raster range 256 × 256 arc sec2, and 20 mÅ spectral resolution in second order. Observations can be made with specific sets of 4 lines simultaneously, or with both sides of 2 lines simultaneously for velocity and polarization. A rotatable retarder can be inserted into the spectrometer beam for measurement of Zeeman splitting and linear polarization in the transition region and chromosphere. Title: Formation of the Solar OI Lines - Implications of an Improved 3D Branching Ratio Authors: Skelton, D. L.; Shine, R. A. Bibcode: 1979BAAS...11..641S Altcode: No abstract at ADS Title: Pre-Flight Calibration of the Solar Maximum Mission Ultraviolet Spectrometer and Polarimeter I. Instrumentation &Spectrometer Performance Authors: Michalitsianos, A. G.; Kenney, P. J.; Shine, R. A.; Woodgate, B. E.; Bruner, E. C., Jr.; Henze, W.; Tandbaer-Hanssen, E. Bibcode: 1979BAAS...11..447M Altcode: No abstract at ADS Title: Pre-Flight Calibrations of Solar Maximum Missions Ultraviolet Spectrometer &Polarimeter II: Polarimeter Performance Authors: Shine, R. A.; Kenny, P. J.; Michalitsianos, A. G.; Woodgate, B. E.; Bruner, E. C.; Rehse, R. A.; Henze, W.; Tandberg-Hanssen, E. Bibcode: 1979BAAS...11..447S Altcode: No abstract at ADS Title: Solar maximum ultraviolet spectrometer and polarimeter Authors: Tandberg-Hanssen, E.; Woodgate, B. E.; Brandt, J. C.; Chapman, R. D.; Hyder, C. L.; Michalitsianos, A. G.; Shine, R. A.; Athay, R. G.; Beckers, J. M.; Bruner, E. C. Bibcode: 1979SPIE..184..264T Altcode: The objectives of the UVSP experiment are to study solar ultraviolet radiations, particularly from flares and active regions, and to measure constituents in the terrestrial atmosphere by the extinction of sunlight at satellite dawn and dusk. The instrument is designed to observe the Sun at a variety of spectral and spatial resolutions in the range from 1150 to 3600 A. A Gregorian telescope with effective focal length of 1.8 m is used to feed a 1 m Ebert-Fastie spectrometer. A polarimeter containing rotatable magnesium fluoride waveplates is included behind the spectrometer entrance slit and will allow all four Stokes parameters to be determined. Velocities on the Sun can also be measured. The instrument is controlled by a computer which can interact with the data stream to modify the observing program. The observing modes, including rasters, spectral scans, velocity measurements, and polarimetry, are also described along with plans for mission operations, data handling, and analysis of the observations. Title: Overlapping emission peaks in the solar C I multiplet at lambda 1560 and lambda 1657. Authors: Shine, R. A.; Lites, B. W.; Chipman, E. G. Bibcode: 1978ApJ...224..247S Altcode: Observations of the C I multiplets at 1560 and 1657 A made with the University of Colorado spectrometer on the OSO 8 satellite are presented and compared with computed profiles for the Vernazza-Avrett-Loeser solar atmosphere. These are optically thick emission lines formed in the solar chromosphere that show the central reversals typical of such lines. In each multiplet there is an interesting case of overlapping emission peaks which shows that such peaks do not constructively combine but instead weaken. This behavior is easily understood and reproduced with an optically thick, non-LTE mode of formation for these lines and is not consistent with an optically thin mechanism. We also find that the shapes of these blends are very sensitive to the magnitude of the nonthermal microvelocities. Title: Line formation in the solar chromosphere. I. The C II resonance lines observed with OSO 8. Authors: Lites, B. W.; Shine, R. A.; Chipman, E. G. Bibcode: 1978ApJ...222..333L Altcode: The temperature structure of the upper chromosphere is investigated using center-to-limb measurements of the C II resonance lines at 1335 A from the University of Colorado spectrometer aboard OSO 8. Spectrum synthesis of these lines shows them to be extremely sensitive to the temperature and the physical extent of the 20,000 K plateau proposed by Vernazza et al (1973). Hydrostatic equilibrium models of the quiet chromosphere are computed to obtain theoretical spectra of the Lyman lines and continuum as well as the center-to-limb behavior of the C II lines. Good agreement is found with observations for a plateau at 16,500 K with about 25% more material than that of Vernazza et al. Title: Analysis of the chromospheric spectrum of O I in Arcturus. Authors: Haisch, B. M.; Linsky, J. L.; Weinstein, A.; Shine, R. A. Bibcode: 1977ApJ...214..785H Altcode: The ultraviolet and near-infrared spectra of O I in Arcturus are analyzed by a 15-level 14-transition model for O I and the Ayres-Linsky (1975) model chromosphere. It is found that the anomalously bright O I resonance lines at 1302, 1305, and 1306 A can be readily explained by a Ly-beta-pumped fluorescence mechanism as originally proposed by Bowen (1974). Observed equivalent widths of the near-infrared triplet and singlet lines are also consistent with the model predictions, but the intercombination lines at 1355 and 1359 A and near-infrared quintet lines may pose a problem. Title: Center-to-Limb Profiles and Spatial Variations of SiII and FeII Lines in the Solar EUV. Authors: Shine, R. A.; Lites, B. W. Bibcode: 1977BAAS....9R.325S Altcode: No abstract at ADS Title: Solar Prominence Line Profiles Observed in the Ultraviolet from OSO-8. Authors: Hansen, E. R.; Schaffner, S. V. H.; Shine, R. A.; Orrall, F. Q. Bibcode: 1977BAAS....9..314H Altcode: No abstract at ADS Title: Formation of the Solar OI Lines at λ13 and λ1355. Authors: Skelton, D. L.; Shine, R. A. Bibcode: 1977BAAS....9Q.325S Altcode: No abstract at ADS Title: Erratum: "Evidence for a corona of Beta Geminorum" [Astrophys. J., Lett., Vol. 193, p. L107 - L110 (1974)]. Authors: Gerola, H.; Linsky, J. L.; Shine, R.; McClintock, W.; Henry, R. C.; Moos, H. W. Bibcode: 1977ApJ...218L..32G Altcode: No abstract at ADS Title: Preliminary results from the Orbiting Solar Observatory 8: transition-zone dynamics over a sunspot. Authors: Bruner, E. C., Jr.; Chipman, E. G.; Lites, B. W.; Rottman, G. J.; Shine, R. A.; Athay, R. G.; White, O. R. Bibcode: 1976ApJ...210L..97B Altcode: No abstract at ADS Title: Preliminary results from the Orbiting Solar Observatory 8: velocities in the solar chromosphere observed in the Si II lambda 1816 line. Authors: Chipman, E. G.; Bruner, E. C., Jr.; Shine, R. A.; Lites, B. W.; Rottman, G. J.; Athay, R. G.; White, O. R. Bibcode: 1976ApJ...210L.103C Altcode: No abstract at ADS Title: Preliminary results from the Orbiting Solar Observatory 8: observations of optically thin lines. Authors: Shine, R. A.; Roussel-Dupre, D.; Bruner, E. C., Jr.; Chipman, E. G.; Lites, B. W.; Rottman, G. J.; Athay, R. G.; White, O. R. Bibcode: 1976ApJ...210L.107S Altcode: The University of Colorado spectrometer aboard OSO 8 has measured the high temperature C IV resonance lines (at 1548 and 1551 A) and the Si IV resonance lines (at 1393 and 1402 A) formed in the solar chromosphere-corona transition region. Preliminary results include studies of mean profiles, a comparison of cell and network profiles, and the behavior of the lines at the extreme solar limb. Title: Preliminary results from the Orbiting Solar Observatory 8: persistent velocity fields in the chromosphere and transition region. Authors: Lites, B. W.; Bruner, E. C., Jr.; Chipman, E. G.; Shine, R. A.; Rottman, G. J.; White, O. R.; Athay, R. G. Bibcode: 1976ApJ...210L.111L Altcode: No abstract at ADS Title: Analysis of OSO-8 Measurements of the Center-to-Limb Behavior of Solar CII Line Profiles. Authors: Lites, B. W.; Shine, R. A. Bibcode: 1976BAAS....8..501L Altcode: No abstract at ADS Title: Resonance-line transfer with partial redistribution. VIII. Solution in the comoving frame for moving atmospheres. Authors: Mihalas, D.; Shine, R. A.; Kunasz, P. B.; Hummer, D. G. Bibcode: 1976ApJ...205..492M Altcode: The effects of partial frequency redistribution in the scattering process for lines formed in moving atmospheres are analyzed using a general method that allows the transfer equation to be solved in the comoving frame of the gas. The same chromospheric and atomic model studied by Cannon and Vardavas (1974) is employed in the calculations, but a depth scale with logarithmically spaced points is adopted. It is found that in both static and moving atmospheres, the profiles obtained with complete and partial frequency redistribution are virtually identical. The large differences in profiles obtained by Cannon and Vardavas when they used complete and partial redistribution are shown to be spurious (and physically unreal) effects resulting from angle averaging in the observer's frame instead of the comoving frame. Title: Periodic Fluctuations in the Solar Transition Zone Authors: Bruner, E. C., Jr.; Chipman, E. G.; Shine, R. A.; Lites, B. W.; Rottman, G. J.; Orrall, F. Q.; Athay, R. G.; White, O. R. Bibcode: 1976BAAS....8Q.313B Altcode: No abstract at ADS Title: Model Calculations of Chromospheric Lines Observed by OSO-8 Authors: Shine, R. A.; Lites, B. W.; Chipman, E. G.; Rousel-Dupree, D.; Bruner, E. C., Jr.; Rottman, G. J.; Orrall, F. Q.; Athay, R. G.; White, O. R. Bibcode: 1976BAAS....8..331S Altcode: No abstract at ADS Title: Velocities in the Solar Chromosphere Observed in the CII λ1336 Line Authors: Chipman, E. G.; Bruner, E. C., Jr.; Shine, R. A.; Lites, B. W.; Rottman, G. J.; Orrall, F. Q.; White, O. R.; Athay, R. G. Bibcode: 1976BAAS....8..312C Altcode: No abstract at ADS Title: OSO-8 Observations of Mean Vertical Motions in the Solar Transition Region Authors: Roussel-Dupree, D. C.; Shine, R. A.; Chipman, E. G.; Bruner, E. C., Jr.; Lites, B. W.; Rottman, G. J.; Orrall, F. Q.; Athay, R. G.; White, O. R. Bibcode: 1976BAAS....8..312R Altcode: No abstract at ADS Title: An Analysis of the Chromospheric O I Lines in Arcturus Authors: Haisch, B. M.; Linsky, J. L.; Weinstein, A.; Shine, R. Bibcode: 1976BAAS....8..303H Altcode: No abstract at ADS Title: Short Period Chromospheric Oscillations Observed with OSO-8 Authors: Athay, R. G.; White, O. R.; Bruner, E. C., Jr.; Chipman, E. G.; Lites, B. W.; Shine, R. A.; Orrall, F. Q. Bibcode: 1976BAAS....8..312A Altcode: No abstract at ADS Title: Supergranulation Velocity Fields Observed in the Solar Transition Region with OSO-8 Authors: November, L. J.; Toomre, J.; Gebbie, K. B.; Simon, G. W.; Bruner, E. C., Jr.; Chipman, E. G.; Lites, B. W.; Shine, R. A.; Orrall, F. Q.; Athay, R. G.; White, O. R. Bibcode: 1976BAAS....8..311N Altcode: No abstract at ADS Title: Repetitive Brightenings in Active Region Transition Zone Lines as Observed with OSO-8 Authors: Lites, B. W.; Hansen, E. R.; Shine, R. A.; Chipman, E. G.; Bruner, E. C., Jr.; Orrall, F. Q.; Athay, R. G.; White, O. R.; Rottman, G. J. Bibcode: 1976BAAS....8Q.331L Altcode: No abstract at ADS Title: The effect of intermediate-scale motions on line formation. Authors: Shine, R. A. Bibcode: 1975ApJ...202..543S Altcode: The problem of LTE and non-LTE line formation in the presence of nonthermal velocity fields with geometric scales between the microscopic and macroscopic limits is investigated in the cases of periodic sinusoidal and sawtooth waves. For a fixed source function (the LTE case), it is shown that time-averaged line profiles progress smoothly from the microscopic to the macroscopic limits as the geometric scale of the motions increases, that the sinusoidal motions produce symmetric time-averaged profiles, and that the sawtooth motions cause a redshift. In several idealized non-LTE cases, it is found that intermediate-scale velocity fields can significantly increase the surface source functions and line-core intensities. Calculations are made for a two-level atom in an isothermal atmosphere for a range of velocity scales and non-LTE coupling parameters and also for a two-level atom and a four-level representation of Na I line formation in the Harvard-Smithsonian Reference Atmosphere (1971) solar model. It is found that intermediate-scale velocity fields in the solar atmosphere could explain the central intensities of the Na I D lines and other strong absorption lines without invoking previously suggested high electron densities. Title: Diffusion effects on the line intensities of He I and He II in the solar transition region. Authors: Shine, R.; Gerola, H.; Linsky, J. L. Bibcode: 1975ApJ...202L.101S Altcode: A heuristic treatment of diffusion in the solar chromosphere-corona transition region is developed. It is shown that diffusion becomes increasingly important with steeper temperature gradients, in active and quiet regions relative to coronal holes, and with increasing excitation potential. Numerical calculations are made for the resonance lines of He I and He II and show that diffusion can enhance these lines. Thus the helium lines may appear relatively weak in coronal holes due to a weakening of the enhancement mechanism. Most transition region lines will be less affected by diffusion than He I or He II. Title: An Archetype Hydrogen Atmosphere Problem Authors: Athay, R. G.; Mihalas, D.; Shine, R. A. Bibcode: 1975SoPh...45...15A Altcode: Populations for the first three bound states and the continuum of hydrogen are determined for an isothermal, hydrostatic atmosphere at 20 000 K. The atmosphere is treated as being optically thin in the Balmer and Paschen continua and illuminated by continuum radiation at these wavelengths with prescribed radiation temperatures. The atmosphere is optically thick in the 2-1, 3-1, 3-2 and c-1 transitions. Three stages of approximation are treated: radiative detailed balance in the 2-1, 3-1 and 3-2 transitions, Title: Resonance-line transfer with partial redistribution. VII. Angle-dependent redistribution. Authors: Milkey, R. W.; Shine, R. A.; Mihalas, D. Bibcode: 1975ApJ...202..250M Altcode: A method is presented for treating radiative transfer in resonance lines, allowing for the full angle and frequency dependence of redistribution in the scattering process, as seen in the laboratory frame. The case of an equivalent-two-level-atom source function is considered; the problem to be treated is then linear in the radiation field. We apply this method to the Ca II lines in the solar atmosphere, using a redistribution function which takes into account a mixture of coherence in the atom's frame, with Doppler redistribution in the laboratory frame (for atoms which have not suffered an elastic collision), and of complete redistribution in the laboratory frame (for atoms that are collisionally perturbed during the emission process). Both the angle-averaged approximation and the full angle-dependent solution were obtained, and were compared to assess, differentially, the effects of angular redistribution upon the computed line profile and its center-to-limb behavior. For the Ca II line in a homogeneous solar chromosphere the angle-dependent effects are found to be negligible, indicating that one may use angle-averaged redistribution functions when studying partial redistribution effects in line profiles. Title: Resonance line transfer with partial redistribution. VI. The Ca II K-line in solar-type stars. Authors: Shine, R. A.; Milkey, R. W.; Mihalas, D. Bibcode: 1975ApJ...201..222S Altcode: Using model atmospheres for solar-type stars based on scaled temperature distributions, we discuss the effects of partial frequency redistribution on the Ca ii K-line profiles. We show that the partial redistribution calculations lead to a significantly lower intensity at K1 than given by calculations based on the assumption of complete redistribution. This implies that fits to observed fluxes with complete redistribution calculations could tend to underestimate systematically the value of the temperature at the chromospheric temperature minimum. Subject headings: chromospheres, stellar - line formation - radiative transfer Title: High Resolution Spectroscopy From Orbiting Solar Observatory VIII: Transition Zone Dynamics Over a Sunspot Authors: Bruner, E. C., Jr.; Chipman, E. G.; Lites, B. W.; Rottman, G. J.; Shine, R. A.; Athay, R. G.; White, O. R. Bibcode: 1975BAAS....7..522B Altcode: No abstract at ADS Title: Persistent Velocity Fields in the Middle Chromosphere Authors: Lites, B. W.; Bruner, E. C., Jr.; Chipman, E. G.; Shine, R. A.; Rottman, G. J.; White, O. R.; Athay, R. G. Bibcode: 1975BAAS....7..522L Altcode: No abstract at ADS Title: Velocities in the Solar Chromosphere Observed in the Si II λ1816 Line Authors: Chipman, E. G.; Bruner, E. C., Jr.; Shine, R. A.; Lites, B. W.; Rottman, G. J.; White, O. R.; Athay, R. G. Bibcode: 1975BAAS....7..522C Altcode: No abstract at ADS Title: OSO-8 Observations of Optically Thin Lines Authors: Shine, R. A.; Rousell-Dupree, D.; Bruner, E. C., Jr.; Chipman, E. G.; Lites, B. W.; Rottman, G. J.; Athay, R. G.; White, O. R. Bibcode: 1975BAAS....7Q.552S Altcode: No abstract at ADS Title: Resonance line transfer with partial redistribution. IV. A generalized formulation for lines with common upper states. Authors: Milkey, R. W.; Shine, R. A.; Mihalas, D. Bibcode: 1975ApJ...199..718M Altcode: A generalized formulation is given for treating partial redistribution effects in transfer problems in resonance lines with common upper states. The formulation allows explicitly for the possibility that several spectral lines may arise in transitions from a given upper level to several sharp lower levels, including, for example, the ground state and metastable states. Line profiles for the Ca II H and K lines have been calculated, accounting for the partial frequency coherence of scattered photons. These profiles are compared with calculations made with identical atomic and atmospheric models but assuming complete redistribution. Very significant differences between the profiles obtained using these two different physical descriptions of the scattering process are found, and it is now apparent that the assumption of complete redistribution is a serious oversimplification of the actual physical situation. The results question the validity of equating brightness temperatures observed at K1 in stellar spectra with minimum temperatures in stellar chromospheres; it appears likely that such a procedure will systematically underestimate the value of T-min. Title: Resonance Line Transfer with Partial Redistribution. V. The Solar CA II Lines Authors: Shine, R. A.; Milkey, R. W.; Mihalas, Dimitri Bibcode: 1975ApJ...199..724S Altcode: Line profiles for the Ca II H and K lines have been calculated, accounting for the partial frequency coherence of scattered photons. These profiles are compared with calculations made with identical atomic and atmospheric models but assuming complete redistribution. Very significant differences between the profiles obtained using these two different physical descriptions of the scattering process are found, and it is now apparent that the assumption of complete redistribution is a serious oversimplification of the actual physical situation. The partial sredistribution (PRD) results are in substantially better agreement with observation than the complete redistribution (CRD) profiles in describing (a) the center-to-limb behavior of the intensity at K1 and K2, (b) the center-to-limb behavior of the wavelength positions of K1 and K2, and (c) the relative behavior of the H and K profiles, as a function of wavelength, at disk center. Further, we find that we may match the observed absolute intensity at K1 with a minimum chromospheric electron temperature of about 4450 K, and that the HSRA temperature minimum is too low when partial redistribution effects are taken into account. This result raises questions about the validity of equating brightness temperatures observed at K1 in stellar spectra with minimum temperatures in stellar chromospheres; it appears likely that such a procedure will systematically underestimate the value of Tmin. Subject headings: chromosphere, solar - line formation - radiative transfer Title: Resonance line transfer with partial redistribution. III. Mg II resonance lines in solar-type stars. Authors: Milkey, R. W.; Ayres, T. R.; Shine, R. A. Bibcode: 1975ApJ...197..143M Altcode: We discuss the gravity dependence of the Mg II resonance lines calculated with inclusion of effects of partial redistribution in frequency. Using chromospheric models scaled from a solar model, we demonstrate the increased decoupling of the radiation temperature of the k1 feature from the minimum electron temperature in lower-gravity models. The limb darkening of the k-line in the main-sequence model is also discussed. Title: Stellar Upper Photosphere Models Based on the Ca II K-wing. II. The Coherent Scattering Approximation Authors: Ayres, T. R.; Linsky, J. L.; Shine, R. A. Bibcode: 1975BAAS....7..359A Altcode: No abstract at ADS Title: Calculations of Profiles for the CaII H and K Lines Including Partial Redistribution Effects Authors: Shine, R. A.; Milkey, R. W.; Mihalas, D. Bibcode: 1975BAAS....7Q.360S Altcode: No abstract at ADS Title: Diffusion Effects on Line Intensities in the Solar Transition Region Authors: Gerola, H.; Shine, R. A. Bibcode: 1975BAAS....7..366G Altcode: No abstract at ADS Title: A possible width-luminosity correlation of the Ca II K1 and Mg II k1 features. Authors: Ayres, T. R.; Linsky, J. L.; Shine, R. A. Bibcode: 1975ApJ...195L.121A Altcode: Existing high resolution stellar profiles of the Ca II and Mg II resonance lines suggest a possible width-luminosity correlation of the K1 minimum features. It is shown that such a correlation can be simply understood if the continuum optical depth of the stellar temperature minimum is relatively independent of surface gravity as suggested by three stars studied in detail. Title: Evidence for a Corona of Beta Geminorum Authors: Gerola, Humberto; Linsky, Jeffrey L.; Shine, Richard; McClintock, W.; Henry, R. C.; Moos, H. W. Bibcode: 1974ApJ...193L.107G Altcode: A spectrometer was used on the satellite Copernicus to observe a chromospheric L alpha emission from the K0 giant beta Gem at 1218.4 A. This emission appears to be in the corona at temperatures near 260,000 deg K, since the ion it is identified with requires 77.4 eV to be produced. Title: Physical Properties of Solar Chromospheric Plages. II: Chromospheric Plage Models Authors: Shine, R. A.; Linsky, J. L. Bibcode: 1974SoPh...39...49S Altcode: We propose chromospheric models of plages to explain profiles of the Ca II H, K, λl8498, λ8542, and λ8662 lines described in Paper I. These models are consistent with boundary conditions imposed by the photosphere and the Lyman continuum. We find that increasing emission in these lines is consistent with a picture of increasing temperature gradient in the low chromosphere and the resulting increase in pressure and electron density at similar line optical depths. With this picture we suggest how to empirically determine the distribution of chromospheric parameters across the solar disk directly from Ca II filtergrams. We also propose that the high density aspects of solar activity are produced by steep temperature gradients in the low chromosphere and thus by the enhanced heating mechanisms that steepen these gradients. Title: An Upper Photosphere Model for Arcturus (K2 III) Based on Partial Redistribution and the Ca II K-line Inner Wings Authors: Ayers, T. R.; Linsky, J. L.; Shine, R. A. Bibcode: 1974BAAS....6..457A Altcode: No abstract at ADS Title: Stellar Model Chromospheres. H. Procyon (F5 Iv/v) Authors: Ayres, Thomas R.; Linsky, Jeffrey L.; Shine, Richard A. Bibcode: 1974ApJ...192...93A Altcode: 1974ApJ...192...95A No abstract at ADS Title: A facular model based on the wings of the Ca ii lines Authors: Shine, Richard A.; Linsky, Jeffrey L. Bibcode: 1974SoPh...37..145S Altcode: We develop a relatively simple procedure for deriving models of upper photospheric regions based on the damping wings of the Ca II resonance and infrared triplet lines. The procedure is used to derive a facular model but can also be applied to late-type stars. We compare our model to that of Chapman. Title: Evidence for a Corona of β Geminorum with the "Copernicus" Satellite. Authors: McClintock, W.; Linsky, J.; Gerola, H.; Shine, R.; Henry, R. C.; Moos, H. W. Bibcode: 1974BAAS....6..315M Altcode: No abstract at ADS Title: Physical Properties of the Chromospheric-Corona Transition Region Based on OSO-VI Data Authors: Shine, R. A.; Gerola, H. Bibcode: 1974BAAS....6..346S Altcode: No abstract at ADS Title: Non-LTE Line Formation in the Presence of Intermediate Scale Velocity Fields Authors: Shine, R. A. Bibcode: 1974BAAS....6S.294S Altcode: No abstract at ADS Title: Line Profiles and Turbulence Generated by Acoustic Waves in the Solar Chromosphere. II. Contours of the Ca II and Mg II K Lines Authors: Shine, Richard A.; Oster, Ludwig Bibcode: 1973A&A....29....7S Altcode: No abstract at ADS Title: One- and Multi-Component Models of the Upper Photosphere Based on Molecular Spectra. I: The Violet System of CN(0,0) Authors: Mount, George H.; Linsky, Jeffrey L.; Shine, Richard A. Bibcode: 1973SoPh...32...13M Altcode: Spectroheliograms taken in the CN(0, 0) violet band near λ 3883 Å show very small scale network and cell structures with high contrast. The bandhead itself, which is a broad feature due to overlap of several CN lines, allows the diagnostic simplicity of a continuum since motions, magnetic fields, and broadening mechanisms are unimportant. We have obtained spectroheliograms in the bandhead and center-to-limb photoelectric spectra of CN(0, 0) at Kitt Peak National Observatory. From the photoelectric spectra and a detailed analysis of the formation of the CN(0, 0) spectrum we derive a best-fit one-component upper photospheric model differing from that of the HSRA and recommend a change in solar carbon abundance from the HSRA value of logAc = 8.55 to logAc = 8.25. From the calibrated spectroheliograms we consider a multi-component model to account for the observed fine structure intensity variations. Title: Photospheric Models Based on the Wings of the Ca II Lines. Authors: Shine, R. A.; Ayres, T. R. Bibcode: 1973BAAS....5..453S Altcode: No abstract at ADS Title: A simple explanation of the Wilson-Bappu effect. Authors: Ayres, T. R.; Linsky, J. L.; Shine, R. A.; Chipman, E. Bibcode: 1973BAAS....5..364A Altcode: No abstract at ADS Title: The Effect of Small and Large Scale Sine Waves upon Chromospheric Line Profiles Authors: Shine, Richard; Oster, Ludwig Bibcode: 1973BAAS....5T.279S Altcode: No abstract at ADS Title: On the dependence of the two-levelsource function on its own radiation field. Authors: Steinitz, Raphael; Shine, Richard A. Bibcode: 1973MNRAS.162..197S Altcode: The consequences of the universally made assumption that the stimulated emission profile is identical to the absorption profile are quantitatively investigated for a two-level atom with Doppler redistribution. The nonlinear terms arising in the source function are evaluated iteratively. We find that the magnitude of the effects are governed by = (hv/kT - I)-' and are probably completely negligible for visible and UV solar lines. For = 2 effects of 5 per cent are encountered. Larger `s lead to numerical instabilities in the method of solution used. Title: Physical Properties of Solar Plages. Authors: Shine, Richard Alan Bibcode: 1973PhDT........22S Altcode: No abstract at ADS Title: Discovery of upper photospheric temperature inversions or chromospheres in early A stars. Authors: Linsky, J. L.; Shine, R. A.; Ayres, T. R.; Praderie, F. Bibcode: 1973BAAS....5....3L Altcode: No abstract at ADS Title: Discovery of Chromospheres in Early A Stars. Authors: Linsky, J. L.; Shine, R. A.; Ayres, T. R.; Praderie, F. Bibcode: 1973BAAS....5R...3L Altcode: No abstract at ADS Title: Physical Properties of Solar Chromospheric Plages. I. Line Profiles of the Ca II H, K, and Infrared Triplet Lines Authors: Shine, Richard A.; Linsky, Jeffrey L. Bibcode: 1972SoPh...25..357S Altcode: Double pass photoelectric observations are presented of five CaII lines (H, K, 8498 Å, 8542 Å, and 8662 Å) in a number of solar plages of different degrees of activity, quiet regions, and a sunspot. The data are compared with previous work. All five lines show increasing emission together in plages and the least opaque of the infrared triplet lines appears to exhibit core emission prior to the more opaque members of the multiplet. The question of source function equality is considered and the differences and similarities among plage profiles and between plage and quiet profiles are shown qualitatively and quantitatively. Title: Photoelectric Ca II Line Profiles in Solar Plages and a Sunspot and Their Preliminary Interpretation Authors: Shine, Richard A.; Linsky, Jeffrey L. Bibcode: 1972BAAS....4T.391S Altcode: No abstract at ADS