Author name code: house ADS astronomy entries on 2022-09-14 author:"House, Lewis" ------------------------------------------------------------------------ Title: The Ejection of Helical Field Structures through the Outer Corona Authors: House, Lewis L.; Berger, Mitchell A. Bibcode: 1987ApJ...323..406H Altcode: The May 5, 1980 coronal mass ejection observed by the SMM coronagraph polarimeter contained an eruptive prominence with apparent helical structure. After a general discussion of the morphology of this event, the evolution of the prominence structure as it traversed the outer corona is described. Particular attention is given to the distribution of magnetic helicity, a measure of helical structure. This distribution can be inferred by tracking the crossovers between individual filaments within the prominence. The northern leg of the prominence consisted of two braided H-alpha filaments shredded into subfilaments near the top. Much of the helicity in this leg resided in a compact central region. As the prominence rose, the central region unwound by expanding rapidly along the leg. This expansion could arise from both acceleration of the prominence material and spreading of the distribution of helicity along the leg. Title: The type IV burst of 1980 June 29, 0233 UT - Harmonic plasma emission? Authors: Gary, D. E.; Dulk, G. A.; House, L. L.; Illing, R.; Wagner, W. J.; Mclean, D. J. Bibcode: 1985A&A...152...42G Altcode: The coronal transient event of 1980 June 29, 0233 UT, was well observed by the HAO Coronagraph/Polarimeter aboard SMM and at meter radio wavelengths by the Culgoora Radioheliograph. The radio event consisted of a strong Type II (shock wave related) burst followed by weak Type IV (storm) continuum. The authors discuss the details of the Type IV portion of the event in terms of two possible emission mechanisms-plasma emission (at the second harmonic) and gyro-synchrotron emission. They find that gyro-synchrotron emission is a possible mechanism only if more stringent requirements are met, viz., that the density of electrons of energy greater than 10 keV is about 10% of the ambient density, that the average energy is about 40 keV, and that the magnetic field strength at 2.5 solar radii is about 2.8 gauss. The authors conclude that this Type IV event is likely due to plasma emission at the 2nd harmonic of the plasma frequency. Title: Vector Magnetic Fields in Prominences - Part Two Hei d3 Stokes Profiles Analysis for Two Quiescent Prominences Authors: Querfeld, C. W.; Smartt, R. N.; Bommier, V.; Landi Degl'Innocenti, E.; House, L. L. Bibcode: 1985SoPh...96..277Q Altcode: The Stokes components of He I D3 emission in two quiescent prominences, using full spectral profile measurements, are analyzed to derive vector magnetic fields. Two independently developed schemes, based on the Hanle effect, are used for interpretation. They involve solutions of the statistical equilibrium equations for the He I D3 multiplet, including the effect of coherency and full level crossing, which predict the magnetic field dependence of the observed polarization. Derived magnetic field vector solutions for each pair of linear polarization Stokes profiles corresponding to an observational point in the prominence are, intrinsically, not uniquely determined, and a set of possible solutions is usually obtained. However, mutual consistency of these solutions with those independently predicted by the form of the circular polarized component, allow, in almost all cases, rejection of all solutions of a set except one symmetrical pair. Of such a pair, a unique solution can be determined with a high confidence level by reference to independent potential field information. Field vectors are found usually to be close to horizontal and normal to the prominence surface, but extreme exceptions are found. Field values range from 6 G to 60 G. The derived vectorfield configurations and their magnitudes are briefly discussed relative to these prominences and to different quiescent prominence models. Title: Type II bursts, shock waves, and coronal transients - The event of 1980 June 29, 0233 UT Authors: Gary, D. E.; Dulk, G. A.; House, L.; Illing, R.; Sawyer, C.; Wagner, W. J.; McLean, D. J.; Hildner, E. Bibcode: 1984A&A...134..222G Altcode: The metric Type-II solar burst event of June 29, 1980, is characterized on the basis of spatially resolved radioheliograph observations obtained at Culgoora, Australia, and visible-light observations obtained with the coronograph/polarimeter of the SMM satellite. The data are presented in images, diagrams, and graphs and discussed in detail. The Type-II emission is found to arise in the dense moving material behind the transient loops, which have sky-plane width 0.5 solar radius and line-of-sight depth 0.1-0.4 solar radius. A faint arc observed moving ahead of the transient loops at about 900 km/sec and not associated with the Type-II burst is attributed to a shock front, and the compression ratio and Alfven Mach number of the enhanced-density region are estimated as n2/n1 = 1.3-3 and M(A) = 1.2-3. The ambient material at 3 solar radii is determined to have Alfven speed 250-625 km/sec and magnetic-field strength 50-120 mG. The total mass of the event is calculated as 700 Tg; the total magnetic energy of the loops is (1.5-15) x 10 to the 29th ergs. Title: Coronal mass ejections observed during the solar maximum mission: Latitude distribution and rate of occurrence Authors: Hundhausen, A. J.; Sawyer, C. B.; House, L.; Illing, R. M. E.; Wagner, W. J. Bibcode: 1984JGR....89.2639H Altcode: Sixty-five coronal mass ejections have been identified in a systematic examination of white-light coronal images obtained between March and September 1980 by the coronagraph/polarimeter flown on the solar maximum mission spacecraft. These ejections were more uniformly distributed in position angle (or ``projected'' solar latitude) than the similar events observed during the Skylab mission in 1973-1974 27% of the solar maximum mission mass ejections were centered at positions more than 45° from the solar equator. The average rate of occurrence of the observed mass ejections for the entire solar maximum mission epoch, based on the assumption that one coronagraph image per spacecraft orbit is sufficient for detection, was 0.9+/-0.15 per 24-hour day. Application of the same sampling assumption to the Skylab data set leads to a rate of 0.75 per 24-hour day and thus a change in this rate from the Skylab era (on the declining phase of sunspot cycle 20) to solar maximum mission (near the maximum of sunspot cycle 21) of only ~20%. Title: Coronal transients and their interplanetary effects. Authors: Hundhausen, A. J.; Burlaga, L. F.; Feldman, W. C.; Gosling, J. T.; Hildner, E.; House, L. L.; Howard, R. A.; Krieger, A. S.; Kundu, M. R.; Low, B. C.; Sheeley, N. R., Jr.; Steinolfson, R. S.; Stewart, R. T.; Stone, R. G.; Wu, S. T. Bibcode: 1984NASRP1120....6H Altcode: Contents: 1. Introduction. 2. Background material: Ancient history - solar flares and geomagnetic storms. Modern history - interplanetary shock waves. Coronal transients or mass ejections. 3. The present: Theoretical models. New observations of coronal mass ejections. 4. The future: Solar origins. Interplanetary effects. Title: Vector Magnetic Fields in Prominences: Observations and Analysis Authors: Smartt, R. N.; House, L. L. Bibcode: 1984KodOB...4...35S Altcode: Stokes polarimeter spectral profiles of He I D3, representing many observational points within a quiescent prominence, are interpreted using a detailed quantum-mechanical theory of resonance polarization for the D3 multiplet. The multiple set of solutions obtained when the linear polarization information alone is used can be reduced, generally to a symmetric pair, when the full, generalized theory is applied that interprets also the weak circular polarization Stokes profile. In most cases a unique solution can be found through additional information available from disk field polarity. Title: Radio and Visible Light Observations of a Coronal Arcade Transient Authors: Gergely, T. E.; Kundu, M. R.; Erksine, F. T., III; Sawyer, C.; Wagner, W. J.; Illing, R.; House, L. L.; McCabe, M. K.; Stewart, R. T.; Nelson, G. J.; Koomen, M. J.; Michels, D.; Howard, R.; Sheeley, N. Bibcode: 1984SoPh...90..161G Altcode: We discuss simultaneous visible-light and radio observations of a coronal transient that occurred on 9 April, 1980. Visible-light observations of the transient and the associated erupting prominence were available from the Coronagraph/Polarimeter carried aboard SMM, the P78-1 coronagraph, and from the Haleakala Observatory. Radio observations of the related type III-II-IV bursts were available from the Clark Lake and Culgoora Observatories. The transient was extremely complex; we suggest that an entire coronal arcade rather than just a single loop participated in the event. Type III burst sources observed at the beginning of the event were located along a nearby streamer, which was not disrupted, but was displaced by the outmoving loops. The type II burst showed large tangential motion, but unlike such sources usually do, it had no related herringbone structure. A moving type IV burst source can be associated with the most dense feature of the white-light transient. Title: A White-Light / Fex / Hα Coronal Transient Observation to 10-SOLAR-RADII Authors: Wagner, W. J.; Illing, R. M. E.; Sawyer, C. B.; House, L. L.; Sheeley, N. R., Jr.; Howard, R. A.; Koomen, M. J.; Michels, D. J.; Smartt, R. N.; Dryer, M. Bibcode: 1983SoPh...83..153W Altcode: Multi-telescope observations of the coronal transient of 15-16 April, 1980 provide simultaneous data from the Solar Maximum Mission Coronagraph/Polarimeter, the Solwind Coronagraph, and the new Emission Line Coronagraph of the Sacramento Peak Observatory. An eruptive prominence-associated white light transient is for the first time seen as an unusual wave or brightening in Fe Xgl6374 (but not in Fe XIVgl5303). Several interpretations of this fleeting enhancement are offered. Title: The association of radio noise storm enhancements with the appearance of additional material in the corona Authors: Kerdraon, A.; Pick, M.; Trottet, G.; Sawyer, C.; Illing, R.; Wagner, W.; House, L. Bibcode: 1983ApJ...265L..19K Altcode: Visible light observations of the corona have been combined with radioheliograph observations at metric wavelengths to examine the dynamic behavior of the corona during and after noise storm onsets and enhancements. For the period studied, the occurrence of such radio events is systematically associated with the addition of coronal material in the vicinity of the radio source. Some of the events correspond to mass ejection transients, but they more frequently represent merely a brightening, which grows in 1 hour or less with the coronal region and remains dense and stable for several hours. Title: Solar radio storms. Proceedings of the 4th CESRA workshop on solar noise storms, held at Trieste, Italy, August 9 - 13, 1982. Authors: Benz, A. O.; Zlobec, P.; Wentzel, D. G.; House, L. L.; Dulk, G. A.; Tlamicha, A.; Melrose, D. B. Bibcode: 1983srs..work.....B Altcode: No abstract at ADS Title: Dynamics of the corona 1.5 to 6 solar radii from SMM. Authors: House, L. L.; Illing, R. M. E. Bibcode: 1983srs..work...99H Altcode: Observations using the coronagraph/polarimeter on board the Solar Maximum Mission satellite have found the corona to be a very active dynamic atmosphere. Significant changes occur in the corona on a variety of time scales ranging from a few hours to a few days. A variety of new phenomena have been observed, including the first direct observations of cool H-alpha material out to 6 R_sun;, impact of a transient on a pre-existing streamer and wave-like motion of rays and the outer portions of streamers. The paper stresses the importance of these observations to interpretation of the source regions of radio noise storms. Title: Visible light observations of a dense plasmoid associated with a moving Type IV solar radio burst Authors: Stewart, R. T.; Dulk, G. A.; Sheridan, K. V.; House, L. L.; Wagner, W. J.; Illing, R.; Sawyer, C. Bibcode: 1982A&A...116..217S Altcode: A coronal transient rising above the eastern limb of the sun was observed simultaneously on April 27, 1980 by the Coronagraph/Polarimeter (C/P) aboard the Solar Maximum Mission spacecraft and by the Culgoora radioheliograph (CRH). The C/P observed an outward-moving loop transient followed by a plasmoid of dense ionized material, while the CRH observed several types of radio bursts, including a moving Type IV burst at 80 MHz whose position coincided with the bright plasmoid. An estimate of the reasonable lower limit of the electron density in the moving Type IV burst indicates that this burst could have resulted from emission at either the fundamental or the second harmonic of the plasma frequency. This is a new result because in the past it was thought that the density in the moving Type IV source region would be too low for plasma radiation. Title: Vector Magnetic Fields in Prominences - Part One - Preliminary Discussion of Polarimeter Observations in he i D3 Authors: House, L. L.; Smartt, R. N. Bibcode: 1982SoPh...80...53H Altcode: A preliminary discussion is presented of measurements of the polarization of the He I D3 multiplet in a quiescent prominence, observed with a wavelength-scanning Stokes polarimeter. For a series of 43 observations in the same prominence, the linear polarization of the major component of D3 lies primarily in the range 1 to 2% and of the wing component, the range 2 to 5%; the polarization vector angle lies primarily in the range 10-25° for the major component, and 25-35° for the other component. From a more limited data set, the polarization of both components is found to first increase as a function of height in the prominence, and then to decrease; the polarization angles of the major component vary in a random-like way with height, while the wing component shows a systematic change. The amount of polarization and the angle of polarization are governed by the Hanle effect. The collective effect of the group of lines at the peak of D3 evidently has a different sensitivity to the Hanle effect than does the wing component, thus yielding at least four independent measurements - two polarizations and two angles. With some redundancy, the vector magnetic field can then be established using the detailed theory of the Hanle effect. Since the wing component of D3 is a simple triplet, an initial estimate of the magnetic field strength and its horizontal orientation, 0, relative to the line of sight, is simply obtained. Examples of such calculations are presented. Title: An association between coronal structures and type III burst sources Authors: Trottet, G.; Pick, M.; House, L.; Illing, R.; Sawyer, C.; Wagner, W. Bibcode: 1982A&A...111..306T Altcode: Observations of the coronal structures overlying type III radio burst producing regions, obtained with the HAO Coronograph/Polarimeter on board the Solar Maximum Mission, have been combined with observations of the type III bursts from the Mark III Nancay Radioheliograph at 169 MHz. A first qualitative comparison of the data, performed for two periods, indicates that the corona overlying type III producing sites is composed of small, discrete, over-dense structures, which are sometimes diverging and short-lived. The type III burst sources are complex, exhibiting elementary components. It is suggested that the type III burst structure follows that of the corona and that discrete structures may play a fundamental role for type III production. Title: Coronal emission-line polarization from the statistical equilibrium of magnetic sublevels. II - Fe XIV 5303 A Authors: House, L. L.; Querfeld, C. W.; Rees, D. E. Bibcode: 1982ApJ...255..753H Altcode: Coronal magnetic fields influence the intensity and linear polarization of light scattered by coronal Fe XIV ions. To interpret polarization measurements of Fe XIV 5303 A coronal emission requires a detailed understanding of the dependence of the emitted Stokes vector on coronal magnetic field direction, electron density, and temperature and on height of origin. The required dependence is included in the solutions of statistical equilibrium for the ion which are solved explicitly for 34 magnetic sublevels in both the ground and four excited terms. The full solutions are reduced to equivalent simple analytic forms which clearly show the required dependence on coronal conditions. The analytic forms of the reduced solutions are suitable for routine analysis of 5303 green line polarimetric data obtained at Pic du Midi and from the Solar Maximum Mission Coronagraph/Polarimeter. Title: Coronal observations from Solar Maximum Mission satellite. Authors: Csoeke-Poeckh, A.; Lee, R. H.; Wagner, W. J.; House, L. L.; Hildner, E.; Sawyer, C. Bibcode: 1982JSpRo..19..345C Altcode: No abstract at ADS Title: Evidence for a shock wave in visible light and radio observations of the 1980 June 29 event Authors: Gary, D. E.; Dulk, G. A.; House, L. L.; Wagner, W. J.; Illing, R. I.; Sawyer, C.; McLean, D. J. Bibcode: 1982AdSpR...2k.253G Altcode: 1982AdSpR...2..253G Shock waves, as evidenced by type II radio bursts, often accompany flares and coronal mass ejection transients. At present, the density enhancements observed by coronagraphs are believed by some to be ejected matter from the low corona, and by others to be the compressed material behind a shock front. If the former is correct, one would expect in some cases to see a density enhancement, associated with the compression region of the shock, some distance ahead of the transient ejecta. Such a density enhancement has not been previously reported.

The coronal transient of 1980 June 29 (0233 UT) was observed with the High Altitude Observatory's Coronagraph/Polarimeter aboard SMM. This flare-associated coronal transient event was well observed with the Culgoora Radioheliograph, including a well-developed type II burst. Visible on the coronagraph images is a faint circular arc moving out well ahead of the transient loops. This arc is moving at more than 900 km s-1 while the transient itself is moving at a speed of about 600 km s-1. Both the arc and transient appear to have originated either prior to the X-ray flare or at some height above the flare at the time of the flare. The type II burst observed at Culgoora is associated with the transient loops, and no type II emission is identified with the faint arc.

Due to its great speed, we interpret the faint arc as a manifestation of a shock wave, but also envision a separate shock wave associated with the transient loops as evidenced by the type II emission. Preliminary density measurements are consistent with this interpretation, and show the outer shock wave associated with the faint arc to have a Mach number MA <= 1.7. At present we have no convincing explanation for the lack of a type II burst in association with the arc.

This work was supported in part by NASA through grants NSG-7287 and NAGW-91 to the University of Colorado, Boulder, and S-55989 to the High Altitude Observatory, National Center for Atmospheric Research. The National Center for Atmospheric Research, NCAR, is sponsored by the National Science Foundation. Title: Report of group B - Observational radio/optical phenomena Authors: House, L. L.; Dulk, G. A. Bibcode: 1982srs..work..332H Altcode: No abstract at ADS Title: Dynamics of the corona 1. 5 and 6 solar radii from SMM (review) Authors: House, L. L.; Illing, R. M. E. Bibcode: 1982srs..work...99H Altcode: No abstract at ADS Title: Vector Magnetic Fields in Sunspots - Part One - Weak-Line Observations Authors: Gurman, J. B.; House, L. L. Bibcode: 1981SoPh...71....5G Altcode: Observations of a round, unipolar sunspot in the Zeeman triplet Fe I λ6302.5 with the High Altitude Observatory Stokes Polarimeter are used to derive the vector magnetic field in the spot. The behavior of the magnitude, inclination, and azimuth of the field vector B across the spot is discussed. A linear relation is found between the continuum intensity Ic and the field magnitude B. Title: Hα Ejecta in the Outer Corona Authors: House, L. L.; Illing, R. M. E.; Sawyer, C.; Wagner, W. J. Bibcode: 1981BAAS...13..862H Altcode: No abstract at ADS Title: The Active Corona II: North Sector. Images from the SMM Coronagraph/Polarimeter Authors: Illing, R. M. E.; Wagner, W. J.; House, L. L.; Sawyer, C. Bibcode: 1981BAAS...13..911I Altcode: No abstract at ADS Title: Association of Coronal Transient Phenomena with Disk Flare Activity from SMM Coronagraph/Polarimeter Data Authors: Illing, R. M. E.; House, L. L.; Wagner, W. J.; Sawyer, C. Bibcode: 1981BAAS...13..862I Altcode: No abstract at ADS Title: Inhibition of Coronal Transient Loop Formation in Strong Magnetic Field Authors: Sawyer, C.; Wagner, W. J.; Illing, R. M. E.; House, L. L. Bibcode: 1981BAAS...13..836S Altcode: No abstract at ADS Title: Radio and visible light observations of matter ejected from the sun Authors: Wagner, W. J.; Hildner, E.; House, L. L.; Sawyer, C.; Sheridan, K. V.; Dulk, G. A. Bibcode: 1981ApJ...244L.123W Altcode: An initial set of visible light and radio observations of a coronal transient made with the Coronagraph/Polarimeter experiment on SMM and the radioheliograph at Culgoora, Australia is presented. It is noted that an enormous loop-shaped transient observed on April 7, 1980, exhibited bright material having whiplike, nonradial motions, as well as moving and stationary radio sources. The data make it possible to establish that a moving type IV radio source was located on or very close to the fast-moving loop. The thermal, kinetic, and magnetic energies in the transient are estimated and, for the first time, compared with the radiative energy of the associated flare. Title: Studies of the corona with the Solar Maximum Mission coronagraph/polarimeter Authors: House, L. L.; Wagner, W. J.; Hildner, E.; Sawyer, C.; Schmidt, H. U. Bibcode: 1981ApJ...244L.117H Altcode: The visible wavelength coronagraph/polarimeter on the Solar Maximum Mission (SMM) spacecraft is providing data on the flare processes manifested by coronal transients and on the degree of disruption of the evolutionary corona at the present epoch of the solar activity cycle. Among the first results are the discovery of frequent H-alpha emission from remnants of eruptive prominences in the outer corona and first observations of Fe XIV line emission to 3.2 solar radii. In the early stages of transients, cavities less dense than the ambient corona are occasionally found trailing the transient loops, with the loops being relatively thick and structureless. Some 22 transients have been identified in the initial survey of 52 days of observations; from this sample the preliminary conclusion is that transients during the SMM era (near solar maximum) occur over a wider range of latitude than, but with about the same range of speeds as, transients during the Skylab era (near solar minimum). Title: Frequency &Location of Coronal Transients Observed w/ the Coronagraph/Polarimeter Aboard SMM Satellite Authors: Hildner, E.; Illing, R. M. E.; Wagner, W. J.; House, L. L.; Sawyer, C.; Hyder, C. L. Bibcode: 1981BAAS...13..861H Altcode: No abstract at ADS Title: Coronal observations from the SMM satellite Authors: Csoeke-Poeckh, A.; Lee, R. H.; Wagner, W. J.; House, L. L.; Sawyer, C.; Hildner, E. Bibcode: 1981aiaa.meetQ....C Altcode: The scientific purpose, coronal observations, and the instrument design and control of the Coronagraph/Polarimeter aboard the Solar Maximum Mission (SMM) satellite are discussed. The instruments were made with an optical design using an achromatic objective lens providing a 10 arcsec resolution in imaging and an SEC vidicon detector allowing integration on the low light levels of the corona. The computer control assures flexibility in the observing program to optimize observations of changing solar phenomena and allows rapid response to SMM or ground-commanded solar flare alerts. Title: Description of a Flare/Eruptive Prominence Associated Coronal Transient Authors: Hildner, E.; Sawyer, C. B.; Wagner, W. J.; Illing, R. M. E.; House, L. L.; Fisher, R. R.; McCabe, M. K. Bibcode: 1980BAAS...12Q.902H Altcode: No abstract at ADS Title: Properties of Hα Ejecta Associated with Coronal Transients in the Outer Corona Authors: House, L. L.; Wagner, W. J.; Sawyer, C.; Illing, R. M. E.; Pneuman, G. W. Bibcode: 1980BAAS...12..900H Altcode: No abstract at ADS Title: Visible Light and Radio Observations of the First Coronal Transient Event of 1980 June 29 Authors: Gary, D. E.; Dulk, G. A.; Wagner, W.; Sawyer, C.; House, L.; Stewart, R. T.; McLean, D. Bibcode: 1980BAAS...12..904G Altcode: No abstract at ADS Title: SMM Coronagraph/Polarimeter Synoptic Observations of the Active Sun Corona Authors: Illing, R. M. E.; House, L. L.; Wagner, W. J.; Sawyer, C. Bibcode: 1980BAAS...12..900I Altcode: No abstract at ADS Title: Relationships Between Type II and Moving Type IV Radio Bursts and Coronal Visible Light Transients Authors: Stewart, R. T.; House, L. L.; Wagner, W. J.; Sawyer, C. Bibcode: 1980BAAS...12..898S Altcode: No abstract at ADS Title: Radio and Visible Light Observations of a Coronal Transient Associated with a Prominence Eruption Authors: Gergely, T. E.; Kundu, M. R.; Erskine, F. T.; Sawyer, C.; Wagner, W. J.; Illing, R.; House, L. L.; McCabe, M. K.; Stewart, R. T.; Nelson, G. J. Bibcode: 1980BAAS...12..900G Altcode: No abstract at ADS Title: A Three-Coronagraph Record from 1 to 10 RO of the Energetics of a Coronal Transient Authors: Wagner, W. J.; Sawyer, C.; Illing, R. M. E.; House, L. L.; Querfeld, C. W.; Sheeley, N. R., Jr.; Howard, R. A.; Koomen, M. J.; Michels, D. J.; Smartt, R. N. Bibcode: 1980BAAS...12Q.902W Altcode: No abstract at ADS Title: Asymmetry and nonradiality in coronal transients Authors: Sawyer, C.; Illing, R. M. E.; House, L. L.; Wagner, W. J.; Kopp, R. Bibcode: 1980BAAS...12Q.899S Altcode: No abstract at ADS Title: SMM Coronagraph/Polarimeter Observations of Coronel Transient Manifestations Correlated with Flare Data Authors: House, L. L.; Csoeke-Poeckh, A.; Sawyer, C.; Wagner, W. J.; Hildner, E. Bibcode: 1980BAAS...12Q.535H Altcode: No abstract at ADS Title: The Frequency, Locations, Sizes, and Speeds of Coronal Mass Ejections at the Peak of Solar Cycle 21-Early Results from SMM Authors: Hildner, E.; House, L. L.; Sawyer, C. B.; Wagner, W. J. Bibcode: 1980BAAS...12R.535H Altcode: No abstract at ADS Title: SMM Orbiting Coronagraph-Early Results Authors: Sawyer, C.; Wagner, W. J.; Hildner, E.; House, L. L. Bibcode: 1980BAAS...12Q.531S Altcode: No abstract at ADS Title: Diffuse Density Fronts Moving through the Outer Corona Observed by the HAO Coronagraph/Polarimeter on the Solar Maximum Mission Spacecraft Authors: Wagner, W. J.; Hildner, E.; House, L. L.; Sawyer, C. Bibcode: 1980BAAS...12R.535W Altcode: No abstract at ADS Title: The High Altitude Observatory coronagraph/polarimeter on the Solar Maximum Mission. Authors: MacQueen, R. M.; Csoeke-Poeckh, A.; Hildner, E.; House, L.; Reynolds, R.; Stanger, A.; Tepoel, H.; Wagner, W. Bibcode: 1980SoPh...65...91M Altcode: The High Altitude Observatory Coronagraph/Polarimeter, to be flown on the National Aeronautics and Space Administration's Solar Maximum Mission satellite, is designed to produce images of the solar corona in seven wavelength bands in the visible spectral range. The spectral bands have been chosen to specifically exclude or include `chromospheric' spectral lines, so as to allow discrimination between ejecta at high (coronal) and low (chromospheric) temperatures, respectively. In addition, the instrument features spectral filters designed to permit an accurate color separation of the F and K coronal components, and a narrow band (5.5 Å) filter to observe the radiance and polarization of the Fe XIV 5303 Å line. The effective system resolution is better than 10 arc sec and the instrument images a selected quadrant (or smaller field) on an SEC vidicon detector. The total height range that may be recorded encompasses 1.6 to more than 6.0R (from Sun center). The instrument is pointed independently of the SMM spacecraft, and its functions are controlled through the use of a program resident within the onboard spacecraft computer. Major experimental goals include: (a) Observation of the role of the corona in the flare process and of the ejecta from the flare site and the overlying corona; (b) the study of the direction of magnetic fields in stable coronal forms, and, perhaps, ejecta; and (c) examination of the evolution of the solar corona near the period of solar maximum activity. Title: A spectrum scanning Stokes polarimeter. Authors: Baur, T. G.; House, L. L.; Hull, H. K. Bibcode: 1980SoPh...65..111B Altcode: A photoelectric polarimeter for measuring line profiles in all four Stokes parameters has been built and operates on the SPO 40 cm coronagraph in a joint project with Sacramento Peak Observatory. A description of the optical and electronic systems and the calibration scheme is presented. Performance parameters determined from observations are also given. The polarimeter package consisting of a pair of KDP's, a quarter wave plate, and a polarizing beam splitter is located at the prime focus of the coronagraph. Modulation of the KDP's encodes polarization information into intensity signals that are electronically detected. The scanning of the spectrum, accomplished by rotating the grating, permits Stokes line profiles to be recorded on magnetic tape for processing. The instrument can be used to scan any line from 3900 to 7000 Å with a spectral resolution of 0.01 Å. Polarizations as small as 0.001% are detectable. The polarimeter and observing system are computer controlled. Title: Polarization Measurements of Prominences - Characteristics of Stokes Profiles Authors: Smartt, R. N.; House, L. L. Bibcode: 1979BAAS...11..409S Altcode: No abstract at ADS Title: Stokes Polarimetry of Quiescent Prominences in HeI D3. Authors: House, L. L.; Smartt, R. N. Bibcode: 1979phsp.coll...81H Altcode: 1979IAUCo..44...81H; 1979phsp.conf...81H No abstract at ADS Title: Stokes Polarimetry of Quiescent Prominences in He I D3 Authors: House, L. L.; Smartt, R. N. Bibcode: 1978BAAS...10..672H Altcode: No abstract at ADS Title: Radiative transfer calculated from a Markov chain formalism. Authors: Esposito, L. W.; House, L. L. Bibcode: 1978ApJ...219.1058E Altcode: The theory of Markov chains is used to formulate the radiative transport problem in a general way by modeling the successive interactions of a photon as a stochastic process. Under the minimal requirement that the stochastic process is a Markov chain, the determination of the diffuse reflection or transmission from a scattering atmosphere is equivalent to the solution of a system of linear equations. This treatment is mathematically equivalent to, and thus has many of the advantages of, Monte Carlo methods, but can be considerably more rapid than Monte Carlo algorithms for numerical calculations in particular applications. We have verified the speed and accuracy of this formalism for the standard problem of finding the intensity of scattered light from a homogeneous plane-parallel atmosphere with an arbitrary phase function for scattering. Accurate results over a wide range of parameters were obtained with computation times comparable to those of a standard 'doubling' routine. The generality of this formalism thus allows fast, direct solutions to problems that were previously soluble only by Monte Carlo methods. Some comparisons are made with respect to integral equation methods. Title: The determination of vector magnetic fields from Stokes profiles. Authors: Auer, L. H.; Heasley, J. N.; House, L. L. Bibcode: 1977SoPh...55...47A Altcode: The application of Unno's (1956) solution of the transfer equation for polarized radiation to the determination of thevector magnetic field is investigated. An analysis procedure utilizing non-linear least squares techniques is developed that allows one to automate the reduction of measured spectral profiles of the Stokes parameters to determine the field angles, strength as well as other parameters. The method is applied to synthetic spectra generated using a model solar atmosphere and yields results of remarkably high accuracy. The influence of additional factors upon determination of the vector field are also considered. These factors include effects of asymmetric profiles, magneto-optical effects, magnetic field gradients, unresolved field elements, scattered light, and instrumental noise. Title: Non-LTE line formation in the presence of magnetic fields. Authors: Auer, L. H.; Heasley, J. N.; House, L. L. Bibcode: 1977ApJ...216..531A Altcode: The equations of radiative transfer and statistical equilibrium in the presence of a magnetic field are presented. A general difference equation scheme for solving the vector transfer equation in Stokes parameters, allowing for arbitrary variations of the magnetic field and other quantities, is described. The solution of the Stokes non-LTE problem for Ca II by the complete linearization method is described, and numerical examples of the procedure are presented. Title: Radiative Transfer Calculated from a Markov Chain Formalism Authors: Esposito, L. W.; House, L. Bibcode: 1977BAAS....9R.470E Altcode: No abstract at ADS Title: Coronal emission-line polarization from the statistical equilibrium of magnetic sublevels. I. Fe XIII. Authors: House, L. L. Bibcode: 1977ApJ...214..632H Altcode: A general formulation for the polarization of coronal emission lines is presented, and the physics is illustrated through application of the formulation to the lines of Fe xiii at 10747 and 10798 A. The goal is to present a foundation for the determination of the orientation of coronal magnetic fields from emission-line polarization measurements. The physics of emission-line polarization is discussed using the statistical equilibrium equations for the magnetic sublevels of a coronal ion. The formulation of these equations, which describe the polarization of the radiation field in terms of Stokes parameters, is presented; and the various rate parameters- both radiative and collisional-are considered. The emission Stokes vector is constructed from the solution of the equilibrium equations for a point in the corona where the magnetic field has an arbitrary orientation. From these results, it is possible to discuss the development of a full three-dimensional model for emission-line polarization from the corona in which the temperature, density, and magnetic field structure may have arbitrary distributions. Integration along the line of sight is accounted for. On the basis of this model, a computer code for the calculation of emission-line polarization is briefly described and illustrated with a number of sample calculations for Fe xiii. Calculations are carried out for three-dimensional models that demonstrate the physics of the formation of emission-line polarization and illustrate how the degree of polarization and angle of polarization and their variations over the corona are related to the density and magnetic field structure. The models considered range from simple cases in which the density distribution with height is spherically symmetric and the field is radial or dipole to a complex case in which both the density and magnetic field distributions are derived from realistic three-dimensional distributions for the 1973 eclipse on the basis of K-coronameter measurements for the density and potential-field extrapolation of surface magnetic fields in the corona. Subject headings: atomic processes - polarization - Sun: corona - Sun: magnetic fields - Zeeman effect Title: A spectrum scanning Stokes polarimeter Authors: Baur, T. G.; House, L. L. Bibcode: 1977SPIE..112..209B Altcode: A photoelectric polarimeter for measuring solar spectral line profiles in all four Stokes parameters has been built and operates on a 40 cm coronagraph in a joint project with Sacramento Peak Observatory. A description of the optical and electronic systems and the calibration scheme is presented. Performance parameters determined from observations are also given. The polarimeter package consisting of a pair of KDP's, a quarter wave plate, and a polarizing beam splitter is located at the prime focus of the coronograph. Modulation of the KDP's encodes polarization information into intensity signals that are electronically detected. The scanning of the spectrum, accomplished by rotating the grating, permits Stokes line profiles to be recorded on magnetic tape for processing. The instrument can be used to scan any line from 3900 to 7000 A with a spectral resolution of .01 A. Polarizations as small as .001 percent are detectable. The polarimeter and observing system are computer controlled. Title: A spectral scanning Stokes polarimeter. Authors: Baur, T. G.; House, L. L. Bibcode: 1977oppo.conf..209B Altcode: No abstract at ADS Title: A Confirmation of Strong Small Scale Fields in the Solar Photosphere. Authors: House, L. L.; Baur, T. G.; Elmore, D. E. Bibcode: 1976BAAS....8Q.500H Altcode: No abstract at ADS Title: Observation of Vector Magnetic Fields in Sunspots Authors: House, L. L.; Baur, T. G.; Elmore, D. E.; Auer, L. W.; Gurman, J.; Heasley, J. N. Bibcode: 1976BAAS....8..346H Altcode: No abstract at ADS Title: Division of Solar Physics: 1975. Annual report. Authors: House, L. L. Bibcode: 1976BAAS....8..401H Altcode: No abstract at ADS Title: Initial Operation of a Scanning Stokes Polarimeter Authors: House, L. L.; Baur, T. G.; Hull, H. K. Bibcode: 1975SoPh...45..495H Altcode: 1976SoPh...45..495H A polarimeter capable of obtaining line profiles in the four Stokes parameters is described in its initial operation. A brief description of the instrument and the first sunspot observation is given. Title: Initial Results from a Scanning Stokes Polarimeter Authors: House, L. L.; Baur, T. G.; Hull, H. K. Bibcode: 1975BAAS....7..349H Altcode: No abstract at ADS Title: Non-LTE Line Formation in the Presence of a Magnetic Field Authors: Auer, L. H.; Heasley, J. N.; House, L. L. Bibcode: 1975BAAS....7..349A Altcode: No abstract at ADS Title: A Spectrum Scanning Stokes Polarimeter Authors: Baur, T. G.; House, L. L.; Hull, H. K. Bibcode: 1975BAAS....7..351B Altcode: No abstract at ADS Title: The non-LTE transport equation for polarized radiation in the presence of magnetic fields. I. Formulation. Authors: House, L. L.; Steinitz, R. Bibcode: 1975ApJ...195..235H Altcode: A formulation of the radiative transfer of polarized light under conditions departing from local thermodynamic equilibrium and accounting for the presence of a magnetic field is presented. The formulation is self-consistent in that the equations of statistical equilibrium for magnetic sublevels are also included. The quantum-mechanical derivation of the absorption matrix, the key to the presentation, is derived in detail utilizing the density matrix approach. The polarization of the radiation field is described in terms of the usual Stokes parameters, but the discussion of the Stokes parameters in this paper illustrates their quantum mechanical origin and interpretation. The equation of radiative transfer for the Stokes vector is cast in a form reminiscent of the nonlocal thermodynamic equilibrium (NLTE) scalar equation of transfer, except that the equation is now a vector equation in the Stokes parameters and the source function is a vector function containing the population of magnetic sublevels. Title: The Theory of the Polarization of Coronal Forbidden Lines Authors: House, Lewis L. Bibcode: 1974PASP...86..490H Altcode: A brief review, presented in simplified terms, is given for the theory of the origin of coronal emission-line polarization. A classical view of the scattering problem in terms of harmonic oscillators is first presented where the influence of the magnetic field is demonstrated. The Van Vleck depolarization phenomena is described in these terms. Next, a more precise physical picture of the emission-line polarization is established through a discussion of the Zeeman effect in scattering. Sample results are discussed for three-dimensional coronal emission4ine models based upon the solution of the statistical equilibrium equations for magnetic sublevels of the Fe xiv ion. Finally, comments are directed toward the determination of magnetic fields based upon emission-line polarization observations where both medeling and deconvolution procedures are mentioned. Key words: corona - polarization - magnetic fields - forbidden lines Title: The Stokes Formulation of Non-LTE Radiative Transfer in a Magnetic Field Authors: House, Lewis L.; Steinitz, Raphael Bibcode: 1973ApL....15..129H Altcode: No abstract at ADS Title: Coronal Emission Line Polarization Authors: House, Lewis L. Bibcode: 1972SoPh...23..103H Altcode: A discussion of a program for the computation of coronal emission line polarization is presented. The starting point is a general formulation of the scattering function for magnetic dipole transitions between any two total angular momentum levels, J → J, J ± 1. Illustration of the behavior of the scattering function for different transitions is given. The integration of the scattering function over the solar disk and along the line of sight accounting for arbitrary distribution of magnetic fields as well as an inhomogeneous temperature and density structure of the corona is considered next. Title: The Mueller Matrix for Scattering - Including the Effects of Interference Authors: House, L. L. Bibcode: 1972lfpm.conf...71H Altcode: No abstract at ADS Title: Coronal Emission Line Polarization Authors: House, L. L. Bibcode: 1972lfpm.conf..113H Altcode: No abstract at ADS Title: Empirically Corrected Calculations of Coronal Visible Lines from the 3p^{5}3D Configuration Authors: Wagner, William J.; House, Lewis L. Bibcode: 1971ApJ...166..683W Altcode: A laboratory study of extreme-ultraviolet spectral lines provided empirical data on the 3p23d configuration in high ionization stages of the Ar I sequence. Using a three-electrode spark source with variable inductance, we have identified t elve 3p53d-3p84f transitions in each of the ions V vi to Fe ix. A least-squares procedure gave a fit of Slater integrals, spin-orbit parameters, and interactions of the type aL(L + 1) to the extreme-ultraviolet wavelengths. Using these empirically corrected energy parameters, we recalculated the energy levels of the 3p03d configuration. Within 3p53d, we suggest that six magnetic-dipole transitions may be associated with visible emission lines observed in the solar corona: N3021, Ni xi, 3F3-1D1 X3167, Fe ix, 3F3-0F3; X3534, Fe ix, 3F2-3D2 X3643, Fe ix, 3F3-'D3; 3S01, Ni xi, 3F3-1D2 4359, Fe ix, 3F3-3D2. Title: Solar Superthermal Event Deduced from X-Ray Lines Authors: Blake, Richard L.; House, Lewis L. Bibcode: 1971ApJ...166..423B Altcode: improved identifications are given for the ionization stages of iron that contributed to the 1.91 A emission feature in solar spectra obtained by the NRL group in a 1966 rocket flight. in addition, it is shown that the observed emission requires a two-component model of the coronal condensation in which, over some 100 seconds, one component must have either departures from iaxwellian velocity distributions or differences in ionization and electron temperatures. Title: Coherence Properties of Polarized Radiation in Weak Magnetic Fields Authors: House, L. L. Bibcode: 1971IAUS...43..130H Altcode: No abstract at ADS Title: The resonance fluorescence of polarized radiation - III. The Stokes parameter and circular polarization formulation of the scattering redistribution function. Authors: House, L. L. Bibcode: 1971JQSRT..11..367H Altcode: No abstract at ADS Title: Empirically-corrected calculations of coronal visible lines from the 3p53d configuration. Authors: Wagner, W. J.; House, L. L. Bibcode: 1971BAAS....3T.265W Altcode: No abstract at ADS Title: The resonance fluorescence of polarized radiation - I. The general scattering function. Authors: House, L. L. Bibcode: 1970JQSRT..10..909H Altcode: No abstract at ADS Title: The resonance fluorescence of polarized radiation- II. Scattering in the normal Zeeman triplet (J = 0 - J'' = 1). Authors: House, L. L. Bibcode: 1970JQSRT..10.1171H Altcode: No abstract at ADS Title: A Solar Spicule Model Based Upon Calcium II K Line Radiative Transfer Studies Authors: Avery, Lorne W.; House, Lewis L. Bibcode: 1969SoPh...10...88A Altcode: Monte Carlo radiative transfer techniques are used to develop a height-dependent spicule model based upon a more realistic configuration than has hitherto been considered. The spicule is represented by a uniform cylinder, of finite length, standing vertically upon a plane chromosphere. The observed, limb-darkened, anisotropic chromospheric flux incident upon the cylinder is incorporated into the transfer calculations. Title: The Treatment of Resonance Scattering of Polarized Radiation in Weak Magnetic Fields by the Monte Carlo Technique Authors: House, Lewis L.; Cohen, Leonard C. Bibcode: 1969ApJ...157..261H Altcode: The problem of resonance scattering in a finite medium which is permeated by a uniform magnetic field is described. A parallel beam of unpolarized photons is assumed incident upon the lower surface of the scattering medium, the direction of propagation being perpendicular to the magnetic field Through inclusion of the Hanle effect which influences the phase coherency of the scattering process, it has been possible to treat the case of weak fields for the normal Zeeman triplet. This is in contrast to most studies of the transport of polarized radiation in which a strong field is assumed, giving rise to well-separated Zeeman components. By the Monte Carlo process "photons" are traced through the scattering medium by using the prob- abilistic laws of interaction, and, by counting the "photons" as they exit, line profiles and the degree of polarization are determined. Results are given for viewing the medium both along and perpendicular to the magnetic field. When the medium is optically thin and viewed along the magnetic field, the linear polarization may change from 100 toO per cent because of the Hanle effect. As the optical depth increases, additional depolarization occurs because of multiple scattering, and it is found that an average of oniy five to ten scatterings are required to completely depolarize the radiation essentially independent of the magnetic field strength. Future application of this type of calculation is discussed in relation to quiescent prominences in the solar atmosphere Title: Hartree-Fock Calculations of Coronal Forbidden Lines in the Argon i Iso-Electronic Sequence Authors: Wagner, William J.; House, Lewis L. Bibcode: 1969ApJ...155..677W Altcode: In the Argon i isoelectronic sequence it is highly likely that coronal forbidden visible transitions will be discovered occurring between levels of the lowest excited configuration 3p53d. Hartree-Fock calcula- tions of wavelengths and magnetic dipole and electric quadrupole transition probabilities have been made in the ions Cr vii to Cu xii. In these stages thirty-four forbidden lines are predicted having transition probabilities greater than 1 sec'. Due to large uncertainties inherent in state-of-the-art self-consistent field calculations, the predicted wavelengths have insufficient accuracy at present to allow a unique identification with coronal lines observed at eclipses Title: Theoretical Wavelengths for Ka-TYPE X-Ray Lines in the Spectra of Ionized Atoms (carbon to Copper) Authors: House, Lewis L. Bibcode: 1969ApJS...18...21H Altcode: Theoretical Hartree-Fock calculations have been used to determine wavelengths of Ka-type X-ray transitions in atoms in which a varying number of the outer, shielding electrons have been removed. The atoms treated range from carbon to copper, and for each element all stages of ionization are considered, with the exception, where applicable, of those stages containing electrons beyond the 3d shell. For the light elements, carbon to neon, the influence of term structure is taken into account. In addition to wavelengths, tables are given for configuratioa and term energies, dipole integrals, and relative multiplet strengths. Comparison of the theoretical wavelengths with known normal Ka X-ray lines and with observed or extrapolated lines in helium-like ions shows that the calculations are not in error by more than 5 per cent. An adjustment of the calculations to match the few known wavelengths yields final results that can aid in further laboratory and astronomical studies of the identification of these unusual X-ray lines. Title: Radiative transport in finite homogeneous cylinders by the Monte Carlo technique. Authors: Avery, L. W.; House, L. L.; Skumanich, A. Bibcode: 1969JQSRT...9..519A Altcode: No abstract at ADS Title: The Monte Carlo technique applied to radiative transfer. Authors: House, L. L.; Avery, L. W. Bibcode: 1969JQSRT...9.1579H Altcode: No abstract at ADS Title: Reinterpretation of the Feature at 23.28 Å in Solar Soft-X Spectra Authors: Blake, Richard L.; House, Lewis L. Bibcode: 1968ApJ...154L.141B Altcode: The feature at 23.28 A observed in solar X-ray spectra and previously reported (Blake and House) as probably a Ka-type line of 0 iii is actually an instrumental effect. Other lines, particularly X1.91, suggested by Fritz et a!., are still believed to be Ka-type lines Title: The Monte Carlo Technique Applied to Radiative Transfer Authors: House, L. L.; Avery, L. W. Bibcode: 1968rla..conf..133H Altcode: No abstract at ADS Title: The Treatment of Resonance Scattering of Polarized Radiation in Weak Magnetic Fields by the Monte Carlo Technique Authors: House, L. L.; Cohen, L. C. Bibcode: 1968rla..conf..255H Altcode: No abstract at ADS Title: A Survey of Current Coronal Visible Line Identifications Authors: Wagner, William J.; House, Lewis L. Bibcode: 1968SoPh....5...55W Altcode: A literature search has been made pertaining to the identifications of coronal visible lines. Of over one hundred lines reported seen at eclipses, about forty identifications are widely quoted. Close scrutiny of the literature, however, reveals that only twenty of these identifications are not disputed by one or more authors. Title: An Investigation of Resonance-Line Scattering by the Monte Carlo Technique Authors: Avery, Lorne W.; House, Lewis L. Bibcode: 1968ApJ...152..493A Altcode: The problem of photon diffusion through a purely scattering atmosphere is investigated by means of the Monte Carlo technique for two types of scattering: (1) complete redistribution and (2) coherent scattering in the rest frame of the atom which leads to partially coherent scattering in the external frame. The Monte Carlo techniques are applied to Lyman-a photons generated at a point source at the center of a plane-parallel slab of large optical thickness. The mean number of scatterings required for escape, (N), is computed for both types of scattering. For thick slabs (N) is found to be much greater under partially coherent conditions. As a result the source function should approach the equilibrium value at smaller optical depths than one predicts under complete redistribution. In addition it is found that, under partially coherent scattering, photons tend to diffuse more easily in space, but less easily in frequency than under complete redistribution. Thus for complete redistribution the photons are more likely to remain in the vicinity of their origin until they escape from the atmosphere as the result of a single, large frequency shift Title: Radiation Transport in a Medium with a Magnetic Field. Authors: House, Lewis L. Bibcode: 1968AJS....73S..63H Altcode: The Monte Carlo method has been applied to photon transport in volume simulating quiescent prominence. This volume is taken to be finite in two dimensions, homogeneous, and permeated by a uniform magnetic field. The lower surface of the model prominence is illuminated by a continuum of unpolarized photons which are assumed to undergo pure scattering. There is no thermal generation of photons within the atmosphere for the present model. The model atom assumed produces a normal Zeeman triplet. In this particular case, application can be made to the resonance line 4227A of Cai. By the Monte Carlo method the history of the photon states of polarization ~1,j2, and ir are traced through the multiple scattering process, and emergent line profiles in flux and intensity are constructed. The absorption line as seen looking at the top and the emission lines from the side and bottom of the prominence will be discussed showing the relation between broadening, polarization, and total intensity or flux versus magnetic field, density and dimensions of the prominence. Title: Additional Resonance Lines of Highly Ionized Sulfur, Chlorine, Argon, and Potassium Authors: Deutschman, William A.; House, Lewis L. Bibcode: 1967ApJ...149..451D Altcode: No abstract at ADS Title: Some Intermediate Coupling Transition Probabilities in Ca XV and Fe XIII Authors: House, Lewis L. Bibcode: 1967ApJ...149..211H Altcode: Absolute line strengths and transition probabilities are calculated in the domain of intermediate coupling for the transition array s2p2-sp3 in Ca xv and Fe xiii. The dipole integrals as well as the energy parameters are calculated from the Hartree-Fock program of Dr. Charlotte Froese. Extrapolated wavelengths are given where sufficient empirical data are available; otherwise, theoretical Hartree-Fock energies are used to compute the wavelengths. The results clearly indicate the necessity for the use of intermediate coupling results where coronal statistical equilibrium problems are concerned. Several lines forbidden in LS coupling show strengths comparable to allowed resonance lines and should, therefore, be observable in the extreme ultraviolet spectrum of the solar corona. Title: K-α X-Ray Transitions in the Solar Atmosphere and Laboratory Plasma Authors: Blake, R. L.; House, L. L. Bibcode: 1967ApJ...149L..33B Altcode: No abstract at ADS Title: Erratum: New Inner-Shell Resonance Lines in Highly Ionized Sulfur and Chlorine Authors: Deutschman, William A.; House, Lewis L. Bibcode: 1966ApJ...145..660D Altcode: No abstract at ADS Title: New Inner-Shell Resonance Lines in Highly Ionized Sulfur and Chlorine Authors: Deutschman, William A.; House, Lewis L. Bibcode: 1966ApJ...144..435D Altcode: No abstract at ADS Title: Erratum: the Formation of the Lyman Continuum: Isothermal Atmosphere. Authors: Dietz, R. D.; House, L. L. Bibcode: 1965ApJ...142.1315D Altcode: No abstract at ADS Title: The Formation of the Lyman Continuum: Isothermal Atmosphere. Authors: Dietz, R. D.; House, L. L. Bibcode: 1965ApJ...141.1393D Altcode: We present in this paper some techniques and results which form a basis for analysis of the solar Lyman continuum The source function for an atom with one bound level is derived taking into account the frequency dependence of continuum processes The Eddington transfer equation for Lyman-continuum radiation in an isothermal, constant-density, hydrogen atmosphere is solved numerically. An approximate analytic solution of the problem is also obtained. Title: Laboratory production of the solar iron lines in the vacuum ultra-violet Authors: House, L. L. Bibcode: 1965IAUS...23...27H Altcode: No abstract at ADS Title: Time-Dependent Coronal Ionization. Authors: House, L. L.; Billings, D. E. Bibcode: 1964ApJ...140.1182H Altcode: Time-dependent ionization processes are tested for possible significance under the conditions of a shodk wave passing through the corona. Equations are solved to determine the time variation of ion and electron temperatures. The resulting electron temperature is used to compute the time variation in ionization of iron. The results of these calculations, when compared to observational characteristics of the corona, definitely favor processes in the corona comparable in scale and frequency to those in the photosphere. Title: The laboratory production of solar iron lines in the vacuum ultraviolet Authors: House, Lewis L. Bibcode: 1964AnAp...27..763H Altcode: No abstract at ADS Title: Neon VII and VIII Wavelengths in the Vacuum Ultraviolet. Authors: House, Lewis L.; Sawyer, George A. Bibcode: 1964ApJ...139..775H Altcode: No abstract at ADS Title: Ionization Equilibrium of the Elements from H to Fe. Authors: House, Lewis L. Bibcode: 1964ApJS....8..307H Altcode: Non-thermodynamic equilibrium calculations to determine the relative concentration of the various stages of ionization of the elements from H to Fe are presented. The results are derived from statistical equilibrium equations for simplified atomic models containing only a ground state and continuum for each stage of ionization. Calculations are given for an electron temperature range of logio T(ev) = -0.5 to 3.0. In general, the calculations apply for an electron density n, < 10 . In many cases they are valid for high densities, n, = 1016 or 10 . A table is given which allows one to determine the upper-limIt of n, for any specific case. The same table illustrates the value of n, required before local thermodynamic equilibrium would be valid. Title: Excitation of Chromospheric MG I. Authors: Athay, R. Grant; House, L. L. Bibcode: 1963ApJ...137..601A Altcode: Our earlier analysis of chromospheric Mg I data is extended to discussions of both empirical and theoretical departures from radiative detailed balance in the strong singlet and triplet lines. At 500 km, general agreement between the empirical and theoretical values is obtained for all lines, assuming an isothermal, spherically symmetric atmosphere. At heights of 1000 and 1500 km, however, further evidence is found for strong departures from spherical symmetry. Title: Departures from Thermodynamic Equilibrium in Chromospheric MG i, CA i, and O I. Authors: Athay, R. Grant; House, Lewis L. Bibcode: 1962ApJ...135..500A Altcode: Comparisons of intensities of Mg I and 0 I emission lines in the flash-spectrum of the low chromosphere reveal evidence of marked departures from a Boltzmann distribution of populations of energy levels. These departures are in the same sense as those found earlier for He I, viz , an overpopulation of the levels connected to the ground state through optically forbidden transitions relative to the levels with permitted transitions. A search for a similar effect in the populations of the excited singlets and triplets of Ca I has not indicated a significant departure from a Boltzmann distribution for the levels studied. However, evidence is found that the ratio Ca i/Ca ii is much greater than would be expected in thermodynamic equilibrium. In the case of Mg I, the optical thickness of the chromosphere in the triplet lines is obtained directly from the observed intensity of the forbidden intercombination line X 4571 (33P-31S). Computed populations of energy levels for a model Mg I atom under a range of temperature and density show satisfactory agreement with observational data for choices of chromospheric temperatures and densities consistent with a model departing from spherical symmetry given by Thomas and Athay (1961, chap. 7). Title: Departures from Thermodynamic Equilibrium in Chromospheric Magnesium i, Calcium i, and Oxygen I. Authors: House, Lewis Lundberg Bibcode: 1962PhDT.........1H Altcode: No abstract at ADS Title: The Balmer: Paschen Ratio in the Chromosphere and the Equilibrium Populations of Hydrogen Angular-Momentum States. Authors: House, Lewis L.; Athay, R. Grant; Zirin, Harold Bibcode: 1961ApJ...133..608H Altcode: The work reported in this paper is a test of the hypothesis that the angular-momentum states of hydrogen are not populated according to their statistical weights. The anomalous ratio of the hydrogen Balmer to Paschen lines observed at the 1952 eclipse is investigated in relation to both observations and theoretical calculations. The Paschen decrement is used to test for a reduced population of states of higher angular momentum; such a depopulation of states was previously suggested as accounting for the anomalous ratio. The decrement does not confirm the suggestion. A statistical equilibrium analysis of the angular-momentum states is used to determine departures in the populations from their LTE values. The results indicate that departures are too small to give the observed Balmer: Paschen ratio. An calculation shows that it is reasonable to average together the substates of different angular momentum in hydrogen chromospheric calculations. Title: Departures from Thermodynamic Equilibrium in Chromospheric MgI, CaI, and OI. Authors: House, Lewis L.; Athay, R. Grant Bibcode: 1961AJ.....66U.286H Altcode: Line intensities from the chromospheric flash spectrum observed at the 1952 total eclipse clearly indicate marked departures from LTE in Mgi and Oi. The same is suggested for Cai, but not unambiguously. The following remarks relate only to Mgi. The stronger triplets X5184 and X3838 are influenced by self-absorption for heights below about 2500 km. The forbidden line X4571 is observed, and is shown to be free from self-absorption. Its intensity leads directly to the opacities in the X5 184 and X3838 triplets. At 500 km the radial opacities at line center are T5i94 3 and T3539 7, establishing that the centers of these lines in the Fraunhofer spectrum are chromospheric in origin. The singlet line X5528 is observed to fall off much more rapidly with height than the triplets even in the absence of self-absorption. The singlet to triplet ratios give unambiguous evidence of departures from LTE. At 1000 km, the intensity of X4571 is enhanced relative to X5528 by factors of 20 to 200 for assumed values of Te of 60000 and 10 0000, respectively. Solutions to the statistical equilibrium equations yield populations of energy levels in good agreement with the empirical values for opacities consistent with those in the chromosphere. The departures from LTE in 3'S and 33P are shown to be the same and essentially independent of height. Typical computed values are b3'5~25 at 60000 and 200 at 80000. The departures from LTE in the higher triplet levels are also relatively independent of height. Typical values are b435~1.4 at 60000 and 3.3 at 80000. For the upper level of N5528, 4'd, the departure from LTE depends strongly on height thereby accounting for the steep gradient in the X5528 emission. Title: Oscillator Strength for the 3s3p^{2} ^{2}S-3s^{2} 3p^{2}P Transition in AL I. Authors: Eddy, John A.; House, Lewis L.; Zirin, Harold Bibcode: 1961ApJ...133..299E Altcode: The oscillator strength for the transition 1s22s22p63s23p2 P2i2, 2S1/2 of Al I has been calculated. A potential was obtained which allowed a numerical solution of the equation for the ground- and excited-state wave functions. An f-value of 034 was computed from both the dipole and the momentum matrix elements, using theoretical energy levels This is thought to be a more reliable value than that derived from observed energies.