Author name code: kucera-ales ADS astronomy entries on 2022-09-14 author:"Kucera, Ales" ------------------------------------------------------------------------ Title: The Solar Activity Monitor Network - SAMNet Authors: Erdélyi, Robertus; Korsós, Marianna B.; Huang, Xin; Yang, Yong; Pizzey, Danielle; Wrathmall, Steven A.; Hughes, Ifan G.; Dyer, Martin J.; Dhillon, Vikram S.; Belucz, Bernadett; Brajša, Roman; Chatterjee, Piyali; Cheng, Xuewu; Deng, Yuanyong; Domínguez, Santiago Vargas; Joya, Raúl; Gömöry, Peter; Gyenge, Norbert G.; Hanslmeier, Arnold; Kucera, Ales; Kuridze, David; Li, Faquan; Liu, Zhong; Xu, Long; Mathioudakis, Mihalis; Matthews, Sarah; McAteer, James R. T.; Pevtsov, Alexei A.; Pötzi, Werner; Romano, Paolo; Shen, Jinhua; Temesváry, János; Tlatov, Andrey G.; Triana, Charles; Utz, Dominik; Veronig, Astrid M.; Wang, Yuming; Yan, Yihua; Zaqarashvili, Teimuraz; Zuccarello, Francesca Bibcode: 2022JSWSC..12....2E Altcode: The Solar Activity Magnetic Monitor (SAMM) Network (SAMNet) is a future UK-led international network of ground-based solar telescope stations. SAMNet, at its full capacity, will continuously monitor the Sun's intensity, magnetic, and Doppler velocity fields at multiple heights in the solar atmosphere (from photosphere to upper chromosphere). Each SAMM sentinel will be equipped with a cluster of identical telescopes each with a different magneto-optical filter (MOFs) to take observations in K I, Na D, and Ca I spectral bands. A subset of SAMM stations will have white-light coronagraphs and emission line coronal spectropolarimeters. The objectives of SAMNet are to provide observational data for space weather research and forecast. The goal is to achieve an operationally sufficient lead time of e.g., flare warning of 2-8 h and provide many sought-after continuous synoptic maps (e.g., LoS magnetic and velocity fields, intensity) of the lower solar atmosphere with a spatial resolution limited only by seeing or diffraction limit, and with a cadence of 10 min. The individual SAMM sentinels will be connected to their master HQ hub where data received from all the slave stations will be automatically processed and flare warning issued up to 26 h in advance. Title: Spectropolarimetric Observations of an Arch Filament System with GREGOR Authors: Balthasar, H.; Gömöry, P.; González Manrique, S. J.; Kuckein, C.; Kučera, A.; Schwartz, P.; Berkefeld, T.; Collados, M.; Denker, C.; Feller, A.; Hofmann, A.; Schlichenmaier, R.; Schmidt, D.; Schmidt, W.; Sigwarth, M.; Sobotka, M.; Solanki, S. K.; Soltau, D.; Staude, J.; Strassmeier, K. G.; von der Lühe, O. Bibcode: 2019ASPC..526..217B Altcode: 2018arXiv180401789B We observed an arch filament system (AFS) in a sunspot group with the GREGOR Infrared Spectrograph attached to the GREGOR solar telescope. The AFS was located between the leading sunspot of negative polarity and several pores of positive polarity forming the following part of the sunspot group. We recorded five spectro-polarimetric scans of this region. The spectral range included the spectral lines Si I 1082.7 nm, He I 1083.0 nm, and Ca I 1083.9 nm. In this work we concentrate on the silicon line which is formed in the upper photosphere. The line profiles are inverted with the code 'Stokes Inversion based on Response functions' to obtain the magnetic field vector. The line-of-sight velocities are determined independently with a Fourier phase method. Maximum velocities are found close to the ends of AFS fibrils. These maximum values amount to 2.4 km s-1 next to the pores and to 4 km s-1 at the sunspot side. Between the following pores, we encounter an area of negative polarity that is decreasing during the five scans. We interpret this by new emerging positive flux in this area canceling out the negative flux. In summary, our findings confirm the scenario that rising magnetic flux tubes cause the AFS. Title: Flare-induced changes of the photospheric magnetic field in a δ-spot deduced from ground-based observations Authors: Gömöry, P.; Balthasar, H.; Kuckein, C.; Koza, J.; Veronig, A. M.; González Manrique, S. J.; Kučera, A.; Schwartz, P.; Hanslmeier, A. Bibcode: 2017A&A...602A..60G Altcode: 2017arXiv170406089G
Aims: Changes of the magnetic field and the line-of-sight velocities in the photosphere are being reported for an M-class flare that originated at a δ-spot belonging to active region NOAA 11865.
Methods: High-resolution ground-based near-infrared spectropolarimetric observations were acquired simultaneously in two photospheric spectral lines, Fe I 10783 Å and Si I 10786 Å, with the Tenerife Infrared Polarimeter at the Vacuum Tower Telescope (VTT) in Tenerife on 2013 October 15. The observations covered several stages of the M-class flare. Inversions of the full-Stokes vector of both lines were carried out and the results were put into context using (extreme)-ultraviolet filtergrams from the Solar Dynamics Observatory (SDO).
Results: The active region showed high flaring activity during the whole observing period. After the M-class flare, the longitudinal magnetic field did not show significant changes along the polarity inversion line (PIL). However, an enhancement of the transverse magnetic field of approximately 550 G was found that bridges the PIL and connects umbrae of opposite polarities in the δ-spot. At the same time, a newly formed system of loops appeared co-spatially in the corona as seen in 171 Å filtergrams of the Atmospheric Imaging Assembly (AIA) on board SDO. However, we cannot exclude that the magnetic connection between the umbrae already existed in the upper atmosphere before the M-class flare and became visible only later when it was filled with hot plasma. The photospheric Doppler velocities show a persistent upflow pattern along the PIL without significant changes due to the flare.
Conclusions: The increase of the transverse component of the magnetic field after the flare together with the newly formed loop system in the corona support recent predictions of flare models and flare observations.

The movie associated to Figs. 4 and 5 is available at http://www.aanda.org Title: Propagation of filament and hot plasma through solar atmosphere as observed with ground based and space instruments Authors: Kucera, A. Bibcode: 2017psio.confE..73K Altcode: No abstract at ADS Title: NLTE modeling of a small active region filament observed with the VTT Authors: Schwartz, P.; Balthasar, H.; Kuckein, C.; Koza, J.; Gömöry, P.; Rybák, J.; Heinzel, P.; Kučera, A. Bibcode: 2016AN....337.1045S Altcode: An active region mini-discretionary-filament was observed with the Vacuum Tower Telescope (VTT) in Tenerife simultaneously in the He I infrared triplet using the Tenerife Infrared Polarimeter 1 (TIP 1), in Hα with the TESOS Fabry-Pérot interferometer, and in Ca II 8542 Å with the VTT spectrograph. The spectropolarimetric data were inverted using the HAZEL code and Hα profiles were modelled by solving a NLTE radiative transfer in a simple isobaric and isothermal 2D slab irradiated both from its bottom and sides from the solar surface. It was found that the mini-discretionary-filament is composed of horizontal fluxtubes, along which the cool plasma of T∼10 000 K can flow with very large, even supersonic, velocities. Title: Spectropolarimetric observations of an arch filament system with the GREGOR solar telescope Authors: Balthasar, H.; Gömöry, P.; González Manrique, S. J.; Kuckein, C.; Kavka, J.; Kučera, A.; Schwartz, P.; Vašková, R.; Berkefeld, T.; Collados Vera, M.; Denker, C.; Feller, A.; Hofmann, A.; Lagg, A.; Nicklas, H.; Orozco Suárez, D.; Pastor Yabar, A.; Rezaei, R.; Schlichenmaier, R.; Schmidt, D.; Schmidt, W.; Sigwarth, M.; Sobotka, M.; Solanki, S. K.; Soltau, D.; Staude, J.; Strassmeier, K. G.; Volkmer, R.; von der Lühe, O.; Waldmann, T. Bibcode: 2016AN....337.1050B Altcode: 2016arXiv160901514B Arch filament systems occur in active sunspot groups, where a fibril structure connects areas of opposite magnetic polarity, in contrast to active region filaments that follow the polarity inversion line. We used the GREGOR Infrared Spectrograph (GRIS) to obtain the full Stokes vector in the spectral lines Si I λ1082.7 nm, He I λ1083.0 nm, and Ca I λ1083.9 nm. We focus on the near-infrared calcium line to investigate the photospheric magnetic field and velocities, and use the line core intensities and velocities of the helium line to study the chromospheric plasma. The individual fibrils of the arch filament system connect the sunspot with patches of magnetic polarity opposite to that of the spot. These patches do not necessarily coincide with pores, where the magnetic field is strongest. Instead, areas are preferred not far from the polarity inversion line. These areas exhibit photospheric downflows of moderate velocity, but significantly higher downflows of up to 30 km s-1 in the chromospheric helium line. Our findings can be explained with new emerging flux where the matter flows downward along the field lines of rising flux tubes, in agreement with earlier results. Title: Non-LTE Inversion of Spectropolarimetric and Spectroscopic Observations of a Small Active-region Filament Observed at the VTT Authors: Schwartz, P.; Balthasar, H.; Kuckein, C.; Koza, J.; Gömöry, P.; Rybák, J.; Kučera, A.; Heinzel, P. Bibcode: 2016ASPC..504..205S Altcode: An active region mini-filament was observed by VTT simultaneously in the He<small>I</small> 10 830 Å triplet by the TIP 1 spectropolarimeter, in Hα by the TESOS Fabry-Pérot interferometer, and in Ca <small>II</small> 8542 Å by the VTT spectrograph. The spectropolarimetric data were inverted using the HAZEL code and Hα profiles were modelled solving a NLTE radiative transfer in a simple isobaric and isothermal 2D slab irradiated both from bottom and sides. It was found that the mini-filament is composed of horizontal fluxtubes, along which the cool plasma of T∼10 000 K can flow by very large - even supersonic - velocities. Title: The CoMP-S Instrument at the Lomnický Peak Observatory: Status Report Authors: Kučera, A.; Ambróz, J.; Gömöry, P.; Habaj, P.; Kavka, J.; Kozák, M.; Schwartz, P.; Rybák, J.; Tomczyk, S.; Sewell, S.; Aumiller, P.; Summers, R.; Watt, A. Bibcode: 2016ASPC..504..321K Altcode: The Coronal Multi-channel Polarimeter for Slovakia (CoMP-S) has been installed at the high-altitude Lomnicky Peak Observatory of the Astronomical Institute of SAS (2633 m a.s.l.) in 2011. The instrument was designed and manufactured by HAO/NCAR (Boulder, USA) with a tunable Lyot filter and polarimeter for visible and near IR spectral regions. This instrument is proposed for coronagraphic observations of magnetic and velocity fields in the solar corona and in prominences. A fundamental upgrade of this instrument has been prepared with pair of cameras sensitive in the near IR spectral region in a new camera module. This upgrade is being incorporated to the instrument in course of the year 2014. In this contribution the technical parameters of the final configuration of the CoMP-S instrument containing four cameras, covering both visible and near IR spectral regions, are described. We also present a potential of the CoMP-S instrument for coronagraphic spectro-polarimetric observations of the solar corona and prominences with a capability for sequential measurements of the spectral profiles of all prominent emission lines in spectral region from 500 to 1100 nm. Title: Dual instrument for Flare and CME onset observations - Double solar Coronagraph with Solar Chromospheric Detector and Coronal Multi-channel Polarimeter at Lomnicky stit Observatory Authors: Kucera, Ales; Tomczyk, Steven; Rybak, Jan; Sewell, Scott; Gomory, Peter; Schwartz, Pavol; Ambroz, Jaroslav; Kozak, Matus Bibcode: 2015IAUGA..2246687K Altcode: We report on unique dual instrument developed for simultaneous measurements of velocity and magnetic fields in the solar chromosphere and corona. We describe the technical parameters and capability of the Coronal Multi-channel Polarimeter (CoMP-S) and Solar Chromospheric detector (SCD) mounted at the Double solar coronagraph at Lomnicky Stit Observatory and working simultaneously with strictly parallel pointing of both coronagraphs. The CoMP-S is 2D spectropolarimeter designed for observations of VIS and near-IR emission lines of prominences and corona with operating spectral range: 500 - 1100 nm, sequential measurement of several VIS and near-IR lines. Its field of view is 14 arcmin x 11 arcmin. It consists of 4-stage calcite Lyot filter followed by the ferro-liquid crystal polarizer and four cameras (2 visible, 2 infrared). The capability is to deliver 2D full Stokes I, Q, U, V, using registration with 2 IR cameras (line + background) and 2 VIS cameras (line + background) SCD is a single beam instrument to observe bright chromosphere. It is a combination of tunable filter and polarimeter. Spectral resolution of the SCD ranges from 0.046 nm for observations of the HeI 1083 nm line up to to 25 pm is for observation of the HeI 587.6 nm line. The birefringent filter of the SCD has high spectral resolution, as well as spatial resolution (1.7 arcseconds) and temporal resolution (10 seconds) First results are also reported and discussed. Title: The Košice meteorite fall: Recovery and strewn field Authors: Tóth, Juraj; Svoreň, Ján; BorovičKa, Jiří Spurný, Pavel; Igaz, Antal; Kornoš, Leonard; Vereš, Peter; Husárik, Marek; Koza, Július; Kučera, Aleš Zigo, Pavel; Gajdoš, Štefan; Világi, Jozef; Čapek, David; Krišandová, Zuzana; Tomko, Šdušan; Ilha, Jiří Schunová, Eva; Bodnárová, Marcela; Búzová, Diana; Krejčová, Tereza Bibcode: 2015M&PS...50..853T Altcode: 2015M&PS..tmp..174T We provide the circumstances and details of the fireball observation, search expeditions, recovery, strewn field, and physical characteristics of the Košice meteorite that fell in Slovakia on February 28, 2010. The meteorite was only the 15th case of an observed bolide with a recovered mass and subsequent orbit determination. Despite multiple eyewitness reports of the bolide, only three videos from security cameras in Hungary were used for the strewn field determination and orbit computation. Multiple expeditions of professionals and individual searchers found 218 fragments with total weight of 11.3 kg. The strewn field with the size of 5 × 3 km is characterized with respect to the space distribution of the fragments, their mass and size-frequency distribution. This work describes a catalog of 78 fragments, mass, size, volume, fusion crust, names of discoverers, geographic location, and time of discovery, which represents the most complex study of a fresh meteorite fall. From the analytical results, we classified the Košice meteorite as an ordinary H5 chondrite. Title: Inferring spectral characteristics of the Hα spectral line observed by the DOT Lyot filter Authors: Koza, J.; Rybák, J.; Gömöry, P.; Kučera, A. Bibcode: 2014CoSka..44...43K Altcode: A tunable Lyot filter can serve as a spectroscopic device rendering wide-field 2-D pseudospectroscopy of solar structures and follow-up crude reconstruction of a spectral line profile at each pixel within the field of view. We developed a method of inferring of the Doppler shift, the core intensity, the core width, and the core asymmetry of the Hα spectral line observed by the Lyot filter installed on the Dutch Open Telescope (DOT). The spectral characteristics are inferred through the fitting of five intensity samples, separated from each other by 0.35 Å, by a 4th-order polynomial, a Gaussian, and a parabola. We use the atlas Hα profile as a reference in estimating deviations of the derived spectral characteristics. The Gaussian is the most preferable means for measurements of the Doppler shift with deviations smaller than 1 km s-1. When using the 4th-order polynomial, deviations are within the interval ±2.5 km s-1, but it renders comparable deviations of the core intensity and the width as the Gaussian. The deviations are largely insensitive to the shape of the filter transmission, but depend mostly non-linearly on the Doppler shift. Therefore, they do not cancel out if the spectral characteristics are represented by their relative variations. Results can be used as corrections of spectral characteristics extracted from area-averaged Hα profiles acquired by the DOT Lyot filter. Title: Transmission profile of the Dutch Open Telescope Hα Lyot filter Authors: Koza, J.; Hammerschlag, R. H.; Rybák, J.; Gömöry, P.; Kučera, A.; Schwartz, P. Bibcode: 2014AN....335..409K Altcode: 2017arXiv171209253K Context Accurate knowledge of the spectral transmission profile of a Lyot filter is important, in particular in comparing observations with simulated data. The paper summarizes available facts about the transmission profile of the Dutch Open Telescope (DOT) Hα Lyot filter pointing to a discrepancy between sidelobe-free Gaussian-like profile measured spectroscopically and signatures of possible leakage of parasitic continuum light in DOT Hα images. We compute wing-to-center intensity ratios resulting from convolutions of Gaussian and square of the sinc function with the Hα atlas profile and compare them with the ratios derived from observations of the quiet Sun chromosphere at disk center. We interpret discrepancies between the anticipated and observed ratios and the sharp limb visible in the DOT Hα image as an indication of possible leakage of parasitic continuum light. A method suggested here can be applied also to indirect testing of transmission profiles of other Lyot filters. We suggest two theoretical transmission profiles of the DOT Hα Lyot filter which should be considered as the best available approximations. Conclusive answer can only be given by spectroscopic re-measurement of the filter. Title: Coronal Multi-channel Polarimeter at the Lomnicky Peak Observatory Authors: Schwartz, P.; Ambroz, J.; Gömöry, P.; Kozák, M.; Kučera, A.; Rybák, J.; Tomczyk, S.; Sewell, S.; Aumiller, P.; Summers, R.; Sutherland, L.; Watt, A. Bibcode: 2014IAUS..300..521S Altcode: Coronal Multi-channel Polarimeter (CoMP-S), developed by HAO/NCAR, has been introduced to regular operation at the Lomnicky Peak Observatory (High Tatras in northern Slovakia, 2633 m a.s.l.) of the Astronomical Institute of Slovak Academy of Sciences. We present here the technical parameters of the current version of the instrument and its potential for observations of prominences in the visual and near-IR spectral regions. The first results derived from observations of prominences in the Hα emission line taken during a coordinated observing campaign of several instruments in October 2012 are shown here. Title: Search for Alfvén waves in a bright network element observed in Hα Authors: Koza, J.; Sütterlin, P.; Gömöry, P.; Rybák, J.; Kučera, A. Bibcode: 2013CoSka..43....5K Altcode: 2013arXiv1304.4027K Alfvén waves are considered as potential transporters of energy heating the solar corona. We seek spectroscopic signatures of the Alfvén waves in the chromosphere occupied by a bright network element, investigating temporal variations of the spectral width, intensity, Dopplershift, and the asymmetry of the core of the Hα spectral line observed by the tunable Lyot filter installed on the Dutch Open Telescope. The spectral characteristics are derived through the fitting of five intensity samples, separated from each other by 0.35 Å, by a 4th-order polynomial. The bright network element displays the most pronounced variations of the Dopplershift varying from 0 to 4 km s-1 about the average of 1.5 km s-1. This fact implies a persistent redshift of the Hα core with a redward asymmetry of about 0.5 km s-1, suggesting an inverse-C bisector. The variations of the core intensity up to ±10 % and the core width up to ±5 % about the respective averages are much less pronounced, but still detectable. The core intensity variations lag behind the Dopplershift variations about 2.1 min. The Hα core width tends to correlate with the Dopplershift and anticorrelate with the asymmetry, suggesting that more redshifted Hα profiles are wider and the broadening of the Hα core is accompanied with a change of the core asymmetry from redward to blueward. We also found a striking anticorrelation between the core asymmetry and the Dopplershift, suggesting a change of the core asymmetry from redward to blueward with an increasing redshift of the Hα core. The data and the applied analysis do not show meaningful tracks of Alfvén waves in the selected network element. Title: A quiescent prominence observed in the Hα line by the COMP-S instrument at the Lomnický Peak Observatory Authors: Schwartz, P.; Rybák, J.; Kučera, A.; Kozák, M.; Ambróz, J.; Gömöry, P. Bibcode: 2012CoSka..42..135S Altcode: A prominence above the NEE limb was observed by the COMP-S instrument attached to the ZEISS coronagraph located at the Lomnický Peak Observatory. Observations were carried out on Nov 2, 2011 between 14:01:13 and 14:11:34 UT. The filter of the instrument was tuned during measurements sequentially in five wavelengths within the profile of the Hα line: 0, ±1, ±2 Å around 6563 Å. FWHM of the transmission function of the filter was ∼0.4Å at these wavelengths. Data were not absolutely calibrated, therefore they could be fitted using only a simple cloud model (1D geometry, a complete frequency redistribution, a source function independent of the optical depth) to diagnose the prominence plasma. As five wavelength points in the profile were not enough for an automatic fitting, five positions at the prominence were chosen for the analysis. Observed data from the five positions were simulated using the cloud model and groups of different models were found for each position. It means that the wavelength scale of a step as large as 1 Å when used for the Hα line is not fine enough for estimation of a correct and unique model. Simulating observations using three different finer wavelength scales it was found that the wavelength scale with a step of 0.3 Å and even more finer in the line core (step of 0.1 Å) is already suitable for more precise and unambiguous plasma diagnostics. We also show that for correct plasma diagnostics it is crucial to take into account an effect of a finite width of the transmission function of the filter. If observed data were fitted irrespectively of this important effect, an error in estimated model parameters could exceed even 100 %, except for the Doppler velocities, for which the error would be much smaller, e.g. for velocities up to 20 km s-1 the error is below 1 %. Title: Košice meteorite - recovery and the strew field Authors: Toth, J.; Porubčan, V.; Borovička, J.; Igaz, A.; Spurný, P.; Svoreň, J.; Husárik, M.; Kornoš, L.; Vereš, P.; Zigo, P.; Koza, J.; Kučera, A.; Gajdoš, S.; Világi, J.; Čapek, D.; Šilha, J.; Schunová, E.; Krišandová, Z.; Tomko, D.; Bodnárová, M.; Búzová, D.; Krejčová, T. Bibcode: 2012epsc.conf..708T Altcode: 2012espc.conf..708T The glare of the bolide on the night of February 28, 2010, illuminated streets and interior of apartments, at some places in Eastern Slovakia and Northern Hungary and cannon-like burst or series of low frequency blasts were heard. Due to bad weather, cloudy skies and scatter showers the Central European Fireball Network (operated by Pavel Spurný of the Czech Academy of Sciences) did not take direct optical records of the bolide and also the Slovak Video Meteor Network (operated by Juraj Tóth of Comenius University in Bratislava) did not operate that night so that at first moment it seemed that there were no scientific records available of this event. Fortunately, fast photoelectric sensors on 7 automated fireball stations in the Czech Republic (6) and Austria (1) worked also under cloudy sky and recorded the light curve of the bolide. It enabled to determine the exact time and duration of the event and to estimate its brightness as well. The bolide reached the maximum brightness of at least -18 magnitudes in one huge flare. This light curve was used also for modeling of meteoroid atmospheric fragmentation. Later, several surveillance cameras data were published showing the moment when the night became a day. Three videos from Hungary (Örkény village, Fazzi Daniella and Vass Gábor; Telki village, contact persons Sárneczky Krisztián, Kiss László and Budapest) actually captured the fireball itself. Thanks to calibration of videos by several members of the Hungarian Astronomical Association (MCSE - www.mcse.hu, namely by Igaz Antal) and the trajectory analysis done by Jiří Borovička gave the hope that significant number of meteorite fragments reached the surface. He also calculated the impact area western of the city of Košice in Eastern Slovakia. The data from the Local Seismic Network of Eastern Slovakia (Peter Moczo of the Comenius University) analyzed by Pavel Kalenda confirmed the atmospheric trajectory as well [1]. Title: The LSO/KSO Hα prominence catalogue: cross-calibration of data Authors: Rybák, J.; Gömöry, P.; Mačura, R.; Kučera, A.; Rušin, V.; Pötzi, W.; Baumgartner, D.; Hanslmeier, A.; Veronig, A.; Temmer, M. Bibcode: 2011CoSka..41..133R Altcode: We present work on the extension of the homogeneous prominence catalogue created for the epoch 1967 — 2009 at the Lomnicky Peak Observatory (LSO) by incorporating new data acquired at the Kanzelhöhe Observatory for Solar and Environmental Research (KSO). We use data of 20 Hα prominences observed almost simultaneously at both observatories during four days in August/September 2009 to analyze the significance of differences of the determined parameters used in the Hα prominence catalogue. A reduction of the data from KSO and adaptation of the resulting parameters to fit the parameters of the LSO catalogue confirm that no special homogenization is needed to create a common catalogue data set. Thus, we justified that the LSO catalogue could be extended onward in the future using a more comprehensive database of observations from KSO. Title: Koronálny multikanálový polarimeter pre observatórium Lomnický štít Title: Koronálny multikanálový polarimeter pre observatórium Lomnický štít Title: Coronal multichannel polarimeter for Lomnický štít Observatory. Authors: Rybák, J.; Ambróz, J.; Gömöry, P.; Kozák, M.; Kučera, A.; Tomczyk, S.; Sewell, S.; Summers, R.; Sutherland, L.; Watt, A. Bibcode: 2010nspm.conf..196R Altcode: The contribution presents the process of development and preparation of the Coronal Multi-channel Polarimeter (COMP-S) for the Lomnický štít Observatory of the SAS Astronomy Institute. The design of the device is based on the experience gained in recent years with the CoMP (High Altitude Observatory / NCAR; Boulder, USA) instrument. The device will be a combination of two main optical components: the Lyot tunable filter and polarimeter, and is prepared specifically for one of the 20 cm Zeiss coronagraph at the Lomnický štít Observatory where it will be installed in 2011. CoMP-S will differ from its predecessor in several respects. The most important difference is that CoMP-S will be able to observe the corona and chromospheric emission lines in the wavelength range from 530 to 1083 nm. This feature will be achieved using superachromatic wave plates and dichroic polarizers with wide bandwidth. Furthermore, in the CoMP-S instrument new SWIFT liquid crystals of Meadowlark Optics company will be used as variable retarders instead of nematic liquid crystal retarders (LCVR) which will considerably shorten the measuring process. Ferroelectric liquid crystals will provide measurements of the full Stokes vector with nearly optimal polarization throughout the whole instrument bandwidth. Recently developed sCMOS cameras are to provide diffraction limit resolution of observations, with the 860x680 arc second field and 30-frames-per-second cadence. The device will be used in the Astronomical Observatory of SAS at Lomnický štít primarily for spectrum polarimetry of prominences and coronal loops of the active solar regions. Title: Magnetic loop emergence within a granule Authors: Gömöry, P.; Beck, C.; Balthasar, H.; Rybák, J.; Kučera, A.; Koza, J.; Wöhl, H. Bibcode: 2010A&A...511A..14G Altcode: 2009arXiv0910.4449G
Aims: We investigate the temporal evolution of magnetic flux emerging within a granule in the quiet-Sun internetwork at disk center.
Methods: We combined IR spectropolarimetry of high angular resolution performed in two Fe i lines at 1565 nm with speckle-reconstructed G-band imaging. We determined the magnetic field parameters by a LTE inversion of the full Stokes vector using the SIR code, and followed their evolution in time. To interpret the observations, we created a geometrical model of a rising loop in 3D. The relevant parameters of the loop were matched to the observations where possible. We then synthesized spectra from the 3D model for a comparison to the observations.
Results: We found signatures of magnetic flux emergence within a growing granule. In the early phases, a horizontal magnetic field with a distinct linear polarization signal dominated the emerging flux. Later on, two patches of opposite circular polarization signal appeared symmetrically on either side of the linear polarization patch, indicating a small loop-like structure. The mean magnetic flux density of this loop was roughly 450 G, with a total magnetic flux of around 3 × 1017 Mx. During the ~12 min episode of loop occurrence, the spatial extent of the loop increased from about 1 to 2 arcsec. The middle part of the appearing feature was blueshifted during its occurrence, supporting the scenario of an emerging loop. There is also clear evidence for the interaction of one loop footpoint with a preexisting magnetic structure of opposite polarity. The temporal evolution of the observed spectra is reproduced to first order by the spectra derived from the geometrical model. During the phase of clearest visibility of the loop in the observations, the observed and synthetic spectra match quantitatively.
Conclusions: The observed event can be explained as a case of flux emergence in the shape of a small-scale loop. The fast disappearance of the loop at the end could possibly be due to magnetic reconnection. Title: Analyses of magnetic field structures for active region 10720 using a data-driven 3D MHD model Authors: Wu, S. T.; Wang, A. H.; Gary, G. Allen; Kucera, Ales; Rybak, Jan; Liu, Yang; Vrśnak, Bojan; Yurchyshyn, Vasyl Bibcode: 2009AdSpR..44...46W Altcode: In order to understand solar eruptive events (flares and CMEs) we need to investigate the changes at the solar surface. Thus, we use a data-driven, three-dimensional magnetohydrodynamic (MHD) model to analyze a flare and coronal mass ejection productive active region, AR 10720 on January 15, 2005. The measured magnetic field from Big Bear Solar Observatory (BBSO) digital vector magnetograph (DGVM) was used to model the non-potential coronal magnetic field changes and the evolution of electric current before and after the event occurred. The numerical results include the change of magnetic flux ( Φ), the net electric current ( IN), the length of magnetic shear of the main neutral line ( Lss), the flux normalized measure of the field twist (α={μIN}/{Φ}) with μ being the magnetic permeability. The current helicity ( Hc) injected into the corona and the photospheric surface velocity are also computed. The characteristic parameters of the buildup process before the event and the decay process after the event are investigated and the amount of magnetic energy converted to drive the event is estimated. Title: Solar Convection and Oscillation Interaction Authors: Hanslmeier, A.; Kučera, A.; Rybák, J.; Wöhl, H.; Gömöry, P. Bibcode: 2009CEAB...33...51H Altcode: In this paper we investigate bisectors of solar photospheric lines. The bisectors reflect vertical velocity gradients over the height of line formation and therefore reveal important information about the dynamics in these layers. Their shape and shift is influenced by (a) convective motions, (b) oscillatory motions that can act differently at different photospheric heights. The bisectors are selected from different locations that show mainly a granular evolution or an intergranular evolution. Two selection criteria were applied: continuum intensity (enhanced for granular bisectors, reduced for intergranular bisectors), and full width at half maximum values (enhanced for intergranular bisectors). The results demonstrate how oscillatory motions influence the bisectors as a whole. In the example given a smaller amplitude of oscillations over intergranular areas is indicated. Title: Observational Evidence for Shocks in the Solar Photosphere - New TESOS/VTT Results Authors: Rybak, J.; Kucera, A.; Hanslmeier, A.; Woehl, H.; Wedemeyer-Boehm, S.; Steiner, O. Bibcode: 2008ESPM...12.2.36R Altcode: High-resolution spectroscopic observations recently acquired with the TESOS spectrometer at the Vacuum Tower Telescope (VTT, Observatorio del Teide, Tenerife) are used to test predictions regarding strongly dynamic events in the photosphere as obtained from three-dimensional numerical simulations with the CO5BOLD-code.

Time series of two-dimensional maps of the Fe I 543.4 nm spectral line profile at different centre-to-limb positions are investigated in a statistical sense by comparing the distributions of individual spectral parameters derived from observations with the corresponding distributions from synthesized spectra calculated with the LINFOR3D code from the simulations. Appropriate degradation of the synthesized spectra was applied in order to take the limited spatial resolution of the telescope, seeing effects, and the scattered instrumental light into account.

At the actual spatial resolution of 0.5 arc sec, the statistics show that signatures of the photospheric dynamics, including the most dynamical events like occasional supersonic flows of plasma in the nearly horizontal direction, are very similar in both observations and simulations.

Discrepancies are found only for those spectral parameters (residual line intensity, Doppler line core shifts), which are affected by non-LTE effects, since non-LTE effects are not taken into account in the synthesis of the Fe I 543.4nm spectral line. Title: Multi-wavelength Observations of Dynamic Fibrils in the Upper Photosphere and Chromosphere Authors: Kucera, A.; Beck, Ch.; Gomory, P.; Koza, J.; Woehl, H.; Rybak, J. Bibcode: 2008ESPM...12.2.52K Altcode: Spatial and temporal evolution of dynamic fibrils (DF) as well as coupling with photospheric features was investigated.

The main target were remnants in the active region 10997 on May 28, 2008. We used about 1 hour series of multi wavelength simultaneous observations of the DFs and corresponding photospheric features. The observations were performed with the german Vacuum Tower Telescope equipped with several post-focus instruments. Namely: TESOS (Triple Etalon SOlar Spectrometer) instrument was used in polarimetric mode (VIP=Visual Imaging Polarimeter) to register 2D spectra of the DFs in H-alpha line and in magnetically sensitive Fe I 630.2 nm line. TIP (Tenerife Infrared Polarimeter) mounted on the Echelle spectrograph was used for spectropolarimetric observations of two neutral iron lines at 1.56 micrometers. We scanned 2D area 80" x 5", producing thus 2D maps of intensity, velocity and magnetic field of the low photosphere under the chromospheric fibril field.

Additionally G-band and H-alpha images were registered with high cadence and the supporting data from the TRACE satellite (17.1 nm, WL, Lyman alpha line and 160 nm continuum) are also available. After careful spatial coalignment of 2D maps we first selected numerous DFs in the H-alpha images. Then we investigated temporal evolution of those DFs concerning changes of their dimensions, positions and fluctuations and correlated these characteristics with temporal evolution of the intensities, velocities and magnetic field characteristics observed in the spatially corresponding photosphere. The poster demonstrates the complex observations, data reduction and coalignment and preliminary results on coupling between DFs and underlying photospheric features. Title: Observation of Turbulence in Solar Surface Convection: I. Line Parameter Correlations Authors: Hanslmeier, A.; Kučera, A.; Rybák, J.; Wöhl, H. Bibcode: 2008SoPh..249..293H Altcode: 2008SoPh..tmp...88H By using slit observations of solar photospheric lines shifted by 0.4 arcsec, a 2D field on the Sun was scanned to obtain a 16-minute time series of 2D line-parameter variations. The aim was to investigate in detail the occurrence of turbulence that can be measured by line-width variations extracted from the line profiles. The continuum-intensity variation served as a proxy for granular (bright) and intergranular (dark) areas. The results show that turbulence is not limited to the intergranular space but is also produced by horizontal motions that may become supersonic, leading to turbulence. These motions lead to brightenings, as predicted by theoretical models. Thus, enhanced line-width variations are found to occur in both bright and dark areas. A Sobel filter served to detect the areas where strong gradients in the line parameters occur. By applying this filter to the different line-parameter variations over the 2D field observed, we can determine whether there exists a similarity of these strong-gradient patterns with other parameters that characterize granular motions such as intensity variations or velocity fluctuations. Title: Temporal Variations in Fibril Orientation Authors: Koza, J.; Sütterlin, P.; Kučera, A.; Rybák, J. Bibcode: 2007ASPC..368..115K Altcode: 2007astro.ph..3733K We measure variations in orientation of fourteen dynamic fibrils as a function of time in a small isolated plage and nearby network using a 10-min time sequence of Hα filtergrams obtained by the Dutch Open Telescope. We found motions with average angular velocities of the order of 1 deg min-1 suggesting systematic turning from one limit position to another, particularly apparent in the case of fibrils with lifetimes of a few minutes. Shorter fibrils tend to turn faster than longer ones, which we interpret as due to vortex flows in the underlying granulation that twist magnetic fields. Title: Propagating Waves in the Chromospheric Network Authors: Gömöry, P.; Rybák, J.; Kučera, A.; Curdt, W.; Wöhl, H. Bibcode: 2007ASPC..368..133G Altcode: Wave modulation of ultraviolet emissions originated in and above quiet chromospheric network is studied. In particular, cross-correlation, wavelet analysis and phase difference analysis of the intensities as well as the Doppler shifts of emission lines of He I 584.33 Å (chromosphere), O V 629.73 Å (transition region) and Mg IX 368.07 Å (corona) are employed to study waves at different heights and their direction of propagation. The results are interpreted as evidence of compressive waves that propagate downward from the transition region to the chromosphere in the observed chromospheric network. Different scenarios regarding the origin and source localization of these waves are discussed. Title: The height dependence of temperature velocity correlation in the solar photosphere Authors: Koza, J.; Kučera, A.; Rybák, J.; Wöhl, H. Bibcode: 2007msfa.conf..139K Altcode: 2007arXiv0704.0603K We derive correlation coefficients between temperature and line-of-sight velocity as a function of optical depth throughout the solar photosphere for the non-magnetic photosphere and a small area of enhanced magnetic activity. The maximum anticorrelation of about -0.6 between temperature and line-of-sight velocity in the non-magnetic photosphere occurs at log [tau] 5 = -0.4. The magnetic field is another decorrelating factor along with 5-min oscillations and seeing. Title: Spectral Characteristics of the Photosphere near a Flare Authors: Kučera, A.; Wöhl, H.; Rybák, J.; Wu, S. T.; Wang, A. H. Bibcode: 2007CEAB...31...21K Altcode: We present the temporal evolution of dynamical characteristics of the solar photosphere in an active region near a flare. Namely, spatial and temporal variations of Doppler velocities at different heights in the photosphere mapped by eight photospheric lines are presented for a time span of 45 minutes. The dynamics of the photosphere before and during a flare which occurred nearby is discussed.

We found that downward plasma motions are well pronounced up to 300 km height in the photosphere but did not reach deeper layers. The downward velocities of the plasma motion caused by the flare are about 1.2 km/s and they are channelled in a thin structure - flux-tube with diameter less than 0.8 arcseconds. The velocities are better noticeable in the active parts of the target than in the quiet ones. The magnetic configuration of the active region is compared with the dynamics behaviour. Title: The Height Dependence of Quiet-Sun Photospheric Temperature Fluctuations in Observations and Simulations Authors: Koza, J.; Kučera, A.; Rybák, J.; Wöhl, H. Bibcode: 2006ASPC..354...43K Altcode: We derive rms temperature fluctuations as a function of height throughout the solar photosphere for the non-magnetic photosphere and a small area of enhanced magnetic activity, through semi-empirical inversion based on response functions of a 15-minute time sequence of 118 arcsec-long slit spectrograms taken at disk center. While the observed low photosphere shows small temperature fluctuations (about ≈ 50 K), the sub-photospheric layers and the upper photosphere show larger fluctuations, with similar gradients as in 3-D radiation discretionary-hydrodynamics simulations. However, the observed rms temperature fluctuations are lower than in the simulations at all depths, which we attribute to smearing by atmospheric seeing. Title: A New Method for Comparing Numerical Simulations with Spectroscopic Observations of the Solar Photosphere Authors: Rybák, J.; Kučera, A.; Wöhl, H.; Wedemeyer-Böhm, S.; Steiner, O. Bibcode: 2006ASPC..354...77R Altcode: A method for comparing high-resolution spectroscopic observations of the solar photosphere with numerical simulations of convection in the solar photosphere is presented.

It is based on the comparison of the granular continuum contrast obtained from both the observations and the synthetic spectra, when the latter are calculated from numerical simulations using a particular type of data degradation. This method can be used post facto when a minimum of auxiliary information on characteristics of the telescope/spectrograph and on seeing conditions is available.

Here, the method is applied to results of numerical simulations computed with the CO5BOLD code and high-resolution spectroscopic observations obtained with the VTT on Tenerife. Title: Photospheric modeling through spectral line inversion. Temperature and radial velocity stratifications and fluctuations Authors: Koza, J.; Kučera, A.; Rybák, J.; Wöhl, H. Bibcode: 2006A&A...458..941K Altcode: Aims.We aim to determine average radial stratifications of various physical parameters throughout the solar photosphere at high angular resolution for non-magnetic and magnetic areas and to compare these with standard semiempirical 1D modeling and with 3D hydrodynamics (HD) and magnetohydrodynamics (MHD) simulations.
Methods: .We analyse a 15-min sequence of adaptive-optics spectrograms of very high angular resolution taken at solar disk centre. We split the data between a quiet area and a magnetic one and derive mean temperature and velocity stratifications and fluctuations for these separately by applying LTE inversion based on response functions.
Results: .The mean temperature stratifications in the non-magnetic region agree well with the classical 1D models and the 3D simulations at all heights. However, the observed rms temperature is much lower than in the simulations, the observed mean velocities indicate more upflows, and the observed velocity fluctuations are smaller except in upper layers. Some of the discrepancies are likely to result from remaining smearing by atmospheric seeing and instrumental limitations. The magnetic area shows conspicuous behaviour at large height. We also find evidence of fast low-photosphere downflows in the magnetic area and of enhanced temperature above a small pore.
Title: Study of a Small-Scale Eruptive Event Observed by SOHO/SUMER Authors: Tomasz, F.; Régnier, S.; Schwarz, P.; Rybák, J.; Kucera, A.; Heinzel, P.; Curdt, W.; Wöhl Bibcode: 2006ESASP.617E..79T Altcode: 2006soho...17E..79T No abstract at ADS Title: Multi-Wavelength Observations with High Resolution of a M5.4 Flare from Ground and Space Authors: Kucera, A.; Wöhl, H.; Rybák, J.; Gömöry, P.; Veronig, A. Bibcode: 2006ESASP.617E..68K Altcode: 2006soho...17E..68K No abstract at ADS Title: The Dynamics and Structure of the Solar Atmosphere As Obtained from Combined SUMER/SOHO and TIP2/VTT Observations Authors: Tomasz, F.; Régnier, S.; Schwartz, P.; Rybák, J.; Kucera, A.; Heinzel, P.; Curdt, W.; Wöhl Bibcode: 2006ESASP.617E..78T Altcode: 2006soho...17E..78T No abstract at ADS Title: SOHO/CDS observations of waves above the network Authors: Gömöry, P.; Rybák, J.; Kučera, A.; Curdt, W.; Wöhl, H. Bibcode: 2006A&A...448.1169G Altcode: We analyze temporal variations in the intensities and the Doppler shifts of He i 584.33 Å (chromosphere), O v 629.73 Å (transition region), and Mg ix 368.07 Å (corona) measured in and above chromospheric network near disk center with the Coronal Diagnostic Spectrometer (CDS) onboard the Solar and Heliospheric Observatory (SOHO). There is significant correlation between the He i and O v modulations, with O v intensity leading He i intensity by 27.3 s ± 4.6 s but no significant time shift in the Doppler shift. Cross-correlation between the O v and Mg ix intensities reveals multiple maxima without correlation between their Doppler shifts. Wavelet power analysis gives evidence of intermittent chromospheric and transition-region oscillations with periodicities in the 250-450 s range and of coronal oscillations in the 110-300 s range. Wavelet phase difference analysis shows that the determined time shift between variations of the He i and O v intensities is dominated by waves with about 300 s periodicity. We interpret these results as giving evidence of compressive waves that propagate downward from the transition region to the chromosphere in the particular chromospheric network. We discuss different scenarios regarding origin and source localization of waves, and we speculate on their role in coronal heating above chromospheric network. Title: Acoustic Flux and Turbulence in the Solar Photosphere Authors: Hanslmeier, A.; Kučera, A.; Rybák, J.; Wöhl, H. Bibcode: 2006CEAB...30...11H Altcode: Using slit scans of solar photospheric spectral lines originating in the middle photosphere a 2-D field on the Sun was obtained and the occurrence of acoustic flux is investigated. As proxies for acoustic flux generation enhanced turbulence (measured by fwhm variations) as well as large continuum intensity values are used. The results show that acoustic flux is not limited to the intergranular space and is also produced by horizontal motions that may become supersonic leading to turbulence. These motions lead to brightenings as it was predicted by theoretical models. Title: Influence of the 5-min oscillations on solar photospheric layers. I. Quiet region Authors: Odert, P.; Hanslmeier, A.; Rybák, J.; Kučera, A.; Wöhl, H. Bibcode: 2005A&A...444..257O Altcode: Time series of 1D spectrograms are used to study the influence of the 5-min oscillations on intensity and velocity fields of different layers of the quiet solar photosphere. We study the continuum intensity field along with intensity and corresponding velocity patterns of the mid and upper photosphere, obtained from two Fe lines. Oscillations seem to dominate the intensity and velocity fields of the higher atmospheric layers. Our results confirm the fast decay of the granular intensity structure with height. From correlations of temperature structures at three different photospheric levels we conclude that there are rapid changes of the structures in the lower photosphere, which are valid for the duration of the time series, while for the upper levels changes of the stuctures are fainter and show significant periodic character. The velocity pattern, on the other hand, shows a periodic propagation through the photosphere. The tests of the influence of seeing conditions on the data are considered. Title: Analysis of Dynamics of Loops in AN Active Region Associated with a Small C-Class Flare Authors: Gömöry, P.; Rybák, J.; Kucera, A.; Wöhl, H. Bibcode: 2005ESASP.596E..56G Altcode: 2005ccmf.confE..56G No abstract at ADS Title: Response Functions of Spectral Lines Suitable for Diagnostics of Solar Rotation Authors: Koza, J.; Kučera, A. Bibcode: 2005HvaOB..29...21K Altcode: The response functions for temperature and line-of-sight velocity of the medium-strong Fe II, strong Fe I and weak N II spectral lines are examined. The lines were previously used for determination of the depth dependence of the solar rotation velocity. The positions of local maxima of the response functions to temperature and the calculated optical depths of formation of line cores are confronted. The close coincidence of these quantities is demonstrated and thus verifying the correctness of the optical depth scale of the investigated solar

rotation profile. Title: Analysis of Doppler Shifts of Spectral Lines Obtained by the CDS/SOHO Instrument Authors: Gömöry, P.; Rybák, J.; Kučera, A.; Curdt, W.; Wöhl, H. Bibcode: 2005ASSL..320..203G Altcode: 2005smp..conf..203G No abstract at ADS Title: On the Behaviour of a Blinker in Chromospheric and Transition Region Layers Authors: Tomasz, F.; Rybák, J.; Kučera, A.; Curdt, W.; Wöhl, H. Bibcode: 2005ASSL..320..207T Altcode: 2005smp..conf..207T No abstract at ADS Title: Variability and Dynamics of the Outer Atmospheric Layers in the Quiet Solar Network Authors: Gömöry, P.; Rybák, J.; Kučera, A.; Curdt, W.; Wöhl, H. Bibcode: 2005HvaOB..29...71G Altcode: A detailed study of the temporal evolution of the chromospheric He I 584.33 Å and the transition region O V 629.73 Å emission line intensities of quiet supergranular network of the Sun near disk centre observed with Coronal Diagnostic Spectrometer (CDS) is presented. A wavelet analysis of the 1729 s (28.8 min) long temporal series was performed in order to derive the duration as well as periods of the chromospheric and the transition region oscillations. The He I line intensities show significant power for periods around 300 s (3.3 mHz), which is relevant only in the second half of the observing sequence (between 800 -- 1700 s). The temporal evolution corresponding to the O V line intensities shows strong power around the period of 400 s (2.5 mHz), which is significant during the whole observing sequence as well as the oscillation of lower power for periods of around 250 s (4.0 mHz), which is present only in the middle of the observing sequence (between 700 -- 1300 s). Title: High Resolution Observations of a M5.4 Flare Authors: Kučera, A.; Wöhl, H.; Rybák, J.; Gömöry, P.; Tomasz, F. Bibcode: 2005HvaOB..29..177K Altcode: Hα observations of a M5.4 flare taken in the active region NOAA 10646 with the Vacuum Tower Telescope at Observatório del Teide, Tenerife, on July 13, 2004 are presented. The temporal evolution of the area of the flare and its morphological changes are investigated and discussed. Simultaneous observations of the flare in EUV lines taken with CDS/SOHO instrument are shown and additional data from GOES-10 instrument are compared. Title: Influence of Transition Region Blinker on the Surrounding Chromospheric and Coronal Plasma Authors: Tomasz, F.; Rybák, J.; Kučera, A.; Curdt, W.; Wöhl, H. Bibcode: 2005HvaOB..29..197T Altcode: Results of spectral analysis of a blinker observed in the transition region O VI 1037.63 Å line and in the chromospheric Ly β 1025.72 Å line which were acquired using the SUMER spectrometer are presented. Chromospheric and coronal plasma in the vicinity of the blinker are investigated using also TRACE Ly α, UV continuum and Fe IX channels. It was found that initial release of energy was localized in the transition region and plasma has been spreading from transition region as a bi-directional jet. Energy reached chromosphere ∼60 seconds after primary emission in the o6 line. There were detected enhanced emissions for about 25-38% in the chromospheric Lyα and UV continuum. Spatial extent of the blinker response is 6'' along the slit in the Lyα filtergram what is ∼3'' less than extent of the blinker in the o6 line. Maximum extent of the blinker response is 7.5'' in Lyα filtergram. Although, both Lyα and UV continuum reflect physical conditions in chromosphere, their patterns are completely different: pattern of the blinker response is compact in the Lyα and UV continuum shows non-compact structure below the transition region blinker. Coronal plasma was not influenced by the blinker although plasma moving toward observer was detected in the final phase of evolution of the blinker. Title: Observational Evidences for Heating of the Solar Corona by Nanoflares in the Network Derived from the Transition Region Spectral Lines Authors: Rybák, J.; Kucera, A.; Curdt, W.; Wöhl, H. Bibcode: 2004ESASP.575..529R Altcode: 2004soho...15..529R No abstract at ADS Title: Dynamics of the Quiet Upper Solar Atmosphere in the Network Authors: Gömöry, P.; Rybák, J.; Kucera, A.; Curdt, W.; Wöhl, H. Bibcode: 2004ESASP.575..400G Altcode: 2004soho...15..400G No abstract at ADS Title: Two-dimensional spectroscopic time series of solar granulation Authors: Hanslmeier, A.; Kucera, A.; Rybák, J.; Wöhl, H. Bibcode: 2004SoPh..223...13H Altcode: In this paper we investigate the dynamics of the solar granulation by analyzing time series of 2D spatially highly resolved spectrograms. These were obtained by spatial scans covering a field of 12 8″ × 20″. The advantage of this method is a high spectral resolution, however, the data are not taken simultaneously and to cover the field described above 50 exposures taken sequentially in time are necessary. Therefore, to obtain one map about 2 minutes are required. Plots of the evolution of different line parameters are given as well as the decay of correlation functions. The correlations between the first map of line parameters and successive maps (which are separated by about 2 minutes) were investigated showing a rapid decay down to a correlation coefficient of 0.4 within 4 minutes, the velocity pattern in the field observed varies on smaller time scales. The temporal variation of correlation between the line parameters for the different lines shows a periodic signal related to 5-min oscillations which could not be totally filtered. The evolution of the correlation functions between line parameters is analyzed which gives an error estimate of all correlation values found in the literature. For the first time it is explicitly shown how evolution in a selected photospheric field influences the evolution of granular/intergranular structures. Title: Indications of shock waves in the solar photosphere Authors: Rybák, J.; Wöhl, H.; Kučera, A.; Hanslmeier, A.; Steiner, O. Bibcode: 2004A&A...420.1141R Altcode: High resolution observations of solar granulation near the solar limb are used in a search for hydrodynamic shocks caused by an abrupt braking of the fast (probably supersonic) horizontal flow of the granular plasma towards the intergranular lane. Shock signatures in the spectral line of Fe II 6456.38 Åof one particular observed shock event are investigated in detail. Evolution, amplitude, and spatial relation of the spectral line characteristics of the shock event are in agreement with predictions from numerical simulations for such shock phenomena in the solar photosphere. The dimensions and amplitudes of the observed shock signatures are comparable to predicted values when seeing and instrumental effects as well as a possible obliqueness of the shock front with respect to the observer's line-of-sight are taken into account. The temporal evolution of such an event is observed for the first time. The stable and declining phase of the event were studied for a time period of almost 2 min. A particular relationship was found between the shock event and a nearby G-band bright point located 2'' from the shock event. It is suggestive that the observed shock is a causal consequence of the magnetic flux concentration, traced by the G-band bright point. Such a type of shock can appear outside the flux concentrations as a consequence of a rapid flux-tube motion. Title: On Relations among the Calibrated Parameters of the Transition Region Spectral Line Authors: Rybák, J.; Kucera, A.; Curdt, W.; Wöhl, H. Bibcode: 2004ESASP.547..311R Altcode: 2004soho...13..311R SUMER/SOHO measurements of the O VI 1031.93 Å emission line (280000 K) in the network and internetwork of the transition region of the quiet solar atmosphere are used for a statistical analysis of the calibrated spectral parameters: the central line intensity (energetic units), the line width (m Å) and the Doppler shift (km/s). A detailed procedure is performed in order to determine the absolute wavelength calibration of the spectra and Doppler shifts using simultaneously observed chromospheric O I 1027.44 Å and 1028.15 Å emission lines (10 000K). The spectral parameters of the O VI line are derived for both single and double Gaussian fitting of the line according to the latest findings on the multi-component nature of the transition region line profiles. Reliability of the absolute wavelength calibration and effects of two classes of the transition region transient events - explosive events and blinkers - are discussed in relation to the overall dependencies of the spectral parameters. Title: On Mutual Relation Among the Outer Atmospheric Layers in Network: SOHO/CDS Study Authors: Gömöry, P.; Rybák, J.; Kucera, A.; Curdt, W.; Wöhl, H. Bibcode: 2004ESASP.547..303G Altcode: 2004soho...13..303G SOHO/CDS measurements of emission in the network of the quiet solar atmosphere near disk center were used to derive mutual relations of emission and dynamics in different temperature regimes in/above supergranular network. Cross-correlation functions of the line intensities and the Doppler shifts of the chromospheric line He I 584.3 Å, the transition region line O V 629.7 Å and the coronal line Mg IX 396.1 Å were calculated in order to study relative variability of different atmospheric layers. Relatively high correlations were found between the intensities and the Doppler shifts of the He I and O V lines with two peaks of the intensity correlation function. The maximum value of the correlation of intensities (CC = 0.86) was reached for the zero time lag and the second maximum (CC = 0.78) was obtained for the time lag -190s (O V precedes He I). Only one sharp peak (CC = 0.55) was detected in the Doppler shift correlation function of these lines for the zero time lag. For the correlation of O V and Mg IX intensities one peak (CC = 0.57) of the correlation function was also discovered for the time lag +150s (Mg IX falls behind O V). In contrast, no correlation was obtained for the Doppler shifts of the O V and Mg IX lines. Summarizing we can assume clear relation in energy transfer and/or mass motion between chromosphere and transition region but no relation was found between corona and the lower parts of the solar atmosphere above the particular network under study. Title: Velocity field in the intergranular atmosphere Authors: Kučera, A.; Koza, J.; Bellot Rubio, L. R.; Hanslmeier, A.; Rybák, J.; Wöhl, H. Bibcode: 2004HvaOB..28...19K Altcode: The line-of-sight velocity ľand macroturbulent velocity are studied in the centre of the intergranular space in the solar photosphere. An inversion method is applied to a 4-min time sequence of Stokes I spectra of the 5, 6 and 7 lines observed with high spatial and temporal resolutions at solar disk centre. The results are presented in the form of the functional dependence of ľ(logτ5,t) and (t) on the continuum optical depth τ5 at 500 nm and time t. A ľof several hundreds of meters per second was found in the upper photosphere (logτ5≤-1.5), where the plasma flows away from the observer. On the contrary, upflows directed toward the observer were found in deeper layers (logτ5>-1.5). The typical value of in the centre of the intergranular space is found to be ∼1.7 kms, which is about 0.5 kms greater than in the adjacent granule. Title: SUMER/SOHO and TRACE Study of the Transition Region Blinker Authors: Tomasz, F.; Rybák, J.; Kucera, A.; Curdt, W.; Wöhl, H. Bibcode: 2004ESASP.547..307T Altcode: 2004soho...13..307T The most prominent transient event is presented from an extensive search for the transition region internetwork activity in the quiet solar atmosphere performed by SUMER/SOHO spectrometer and TRACE. SUMER spectra of Ly line (1025.4 Å), two C II lines (1036.3 Å, 1037.0 Å) and O VI line (1037.61 Å) were used for determination of the spatial and temporal evolution of the transient event in the transition region. TRACE images taken in the 1216 Å passband, UV continuum (1700 Å) and Fe IX line (171 Å) were utilized in order to gain information about large-scale coronal structures and small-scale chromospheric variability in the vicinity of the transient event. The main physical and geometrical parameters of the event were derived for the transition region O VI line: the spatial extent of 11 000 km, duration for 9 minutes, intensity enhancement factor of 7 and the Doppler velocities of both signs up to 15 km/s. According to these values the event was identified as a transition region blinker. High deviations of the acquired O VI line profiles from single-Gaussian and some multi-Gaussian profiles reveal dynamics of the event - occurrence of the bidirectional jet which is not typical for blinkers. Besides rapid changes in intensity and in velocity, a rapid increase by a factor of 4.2 was found in the Gaussian width of O VI line as compared to the internetwork. Surrounding chromospheric and coronal structures around the event are discussed on base of the simultaneously taken TRACE images. Title: One-dimensional spectroscopy of the solar photosphere Authors: Odert, P.; Hanslmeier, A.; Rybák, J.; Kučera, A.; Wöhl, H. Bibcode: 2004HvaOB..28...37O Altcode: Data from a time series of spectrograms were used to study correlative relationships between intensity and velocity in the solar photosphere. The variations along the slit of the line parameters from two Fe lines lying in the visible range of the spectrum were used. The formation height difference of these lines is over 300 km. The temporal variations of the correlation coefficients were studied, they showed a strong influence of the 5 min-oscillations. Title: Proper motions of sunspots - new data and further results Authors: Wöhl, H.; Brajša, R.; Kučera, A.; Ruždjak, V.; Rybák, J. Bibcode: 2004HvaOB..28...47W Altcode: The attempts to investigate patterns of motions of main spot components and small pores in complex sunspot groups were continued. The data discussed stem mainly from observations at Hvar/HR and Tatranská Lomnica/SK. Two historic collections of photographic plates are included: The plate archives of the former Fraunhofer Institute and that of photographic plates taken at Skalnate Pleso/SK. Title: The range of reliability of the line-of-sight velocity in a semiempirical model of a granule Authors: Koza, J.; Kučera, A. Bibcode: 2003CoSka..33..224K Altcode: Stokes I response functions to the line-of-sight velocity vLOS of two medium-strong Fe I 522.5 nm and Fe I 557.6 nm lines and the weak line Fe I 557.7 nm have been calculated using a semiempirical 1D model of the granular photosphere affected by 5-min oscillations. A new method is presented allowing to estimate the range of optical depths within which the inferred values of an atmospheric parameter can be considered as reliable. The sensitivity of the individual lines to the variations of vLOS is examined and the range of reliability of vLOS is estimated applying the new method. It is shown that for the given line set the Fe I 522.5 nm line is the most sensitive one and, in turn, the Fe I 557.7 nm line has very low sensitivity to the variations of vLOS. In the case of the Fe I 522.5 nm line the impact of a vLOS perturbation on the intensity of a profile point is about 50% greater than that on the Fe I 557.6 nm line. As a consequence of evolution of the physical conditions in a granule the range of reliability of the model varies and it consists of two separate regions occupying the lower and upper photosphere. Title: Dynamics and turbulence of the chromospheric layers of a flaring atmosphere Authors: Brčeková, K.; Kučera, A.; Hanslmeier, A.; Rybák, J.; Wöhl, H. Bibcode: 2003AN....324..366B Altcode: No abstract at ADS Title: Transition region blinker - spatial and temporal behaviour Authors: Tomasz, F.; Rybák, J.; Kučera, A.; Curdt, W.; Wöhl, H. Bibcode: 2003HvaOB..27...75T Altcode: From an extensive search for transition region internetwork activity in the quiet Sun atmosphere the most prominent transient event is presented. The basic physical and geometrical parameters of this event are derived from the O VI 1037.61 Å emission spectral line. The spatial extent of 11 000 km, duration for 9 minutes, intensity enhancements factor of 7 and large Doppler velocities of both signs were estimated for the event. According to these values this event was identified as a transition region blinker. Title: Proper motions of sunspot groups Authors: Wöhl, H.; Brajša, R.; Kučera, A.; Ruždjak, V.; Rybák, J. Bibcode: 2003HvaOB..27....1W Altcode: Attempts to investigate typical patterns of motions of main spot components and small pores in complex sunspot groups are described. The data used up to now stem from observations at Hvar/HR, Tatranská Lomnica/SK, Izaña/E, Debrecen/H and from the MDI instrument on SoHO. Preliminary results are presented. Title: Evolution of temperature in granule and intergranular space Authors: Koza, J.; Bellot Rubio, L. R.; Kučera, A.; Hanslmeier, A.; Rybák, J.; Wöhl, H. Bibcode: 2003AN....324..349K Altcode: The temporal evolution of temperature in a dissolving granule and in an adjacent intergranular space is presented. The semi-empirical evolutionary models have been calculated using an inversion method applied to 4-min time series of Stokes I spectral line profiles. The models are presented in the form of the functional dependence of temperature T(log tau_5 ,t) on optical depth tau_5 at 500 nm and time t. The observed disappearance of the granule is accompanied with overall cooling of the granular photosphere. Temperature changes greater than 100 K have been found in deeper (log tau_5 >=0) and upper layers (log tau_5 <=-2) whereas the intermediate layers are thermally stable. The intergranular space, which is 2 arcsec off the granule, keeps the temperature structure of the layers from log tau_5 =0.5 to log tau_5 =-2 without global evolutionary changes except short-term and spatially confined heating. Finally, the significant temperature changes in the upper layers (log tau_5 <=-2.5) observed during the time interval of 4 min are found to be typical for the granular and intergranular photosphere. Title: Observational evidence for a shock event in the solar granulation Authors: Kučera, A.; Rybák, J.; Hanslmeier, A.; Wöhl, H. Bibcode: 2003HvaOB..27...25K Altcode: High resolution spectra of Fe II 6456.39 Å line are used to investigate a shock in the solar granulation. The changes of the main spectral characteristics measured in the shock area are in a good agreement with the characteristics predicted with theory. The analysis of the shock, made in the past by several authors was extended in this work to the analysis of a temporal development of the shock event. The 2 minutes duration of a stable and declining phases of the event was studied. We conclude that the observed shock belonged to the particular type of shock generated as a consequence of the swaying motion of the magnetic flux tube concentrated in the intergranular lane. Such type of shock was proposed by numerical simulations made by Steiner et al. 1998. Title: Transition region eruptive event observed with SOHO/CDS in the quiet Sun network Authors: Gömöry, P.; Rybák, J.; Kučera, A.; Curdt, W.; Wöhl, H. Bibcode: 2003HvaOB..27...67G Altcode: CDS observations of the quiet Sun network in the chromospheric He I 584.33 Å and transition region O V 629.73 Å emission lines over a time period of ∼ 29 min are presented. One eruptive event was detected in this time series of data. The parameters of the network eruptive event are derived and the type of this small-scale activity is identified. The lifetime of the event was ∼ 1 min and it was found only in the transition region emission line. This event had no chromospheric counterpart. All O V spectral profiles of the eruptive event were blueshifted and the maximal Doppler shift was -14.7 km s-1. During an initial phase of the eruptive event, the O V intensity enhancement factor was 2.3. These parameters indicate that the observed event could be a transition region explosive event but measured with the limited resolution of the CDS instrument. Title: Line intensities of chromospheric and photospheric spectra of a flare Authors: Brčeková, K.; Kučera, A.; Hanslmeier, A.; Rybák, J.; Wöhl, H. Bibcode: 2002ESASP.506..557B Altcode: 2002ESPM...10..557B; 2002svco.conf..557B In this work we present the intensities of spectral lines determined from the time series of high resolution spectra obtained during the relaxing phase of subflare. The spectra were taken in the core of chromospheric Ca II K line and in two photospheric Fe I 522.5 nm and Fe I 557.6 nm lines. It is shown, that the energy of the flaring chromosphere slightly affects the underlying photospheric layers by heating a small area right under the core of the subflare. Title: Two-dimensional spectroscopic time series of solar granulation: evolution of individual granules Authors: Hanslmeier, Arnold; Kučera, Ales; Rybák, Jan; Wöhl, Hubertus Bibcode: 2002ESASP.506..633H Altcode: 2002svco.conf..633H; 2002ESPM...10..633H In this paper we investigate the dynamics of the solar granulation by analyzing time series of 2-D spatially highly resolved spectrograms. The high quality of the data permitted us to follow the evolution of individual granular and intergranular areas. We used scans over the solar surface in order to obtain a 2-D information. This has the advantage of achieving high spectral and spatial resolution, however one scan lasted for about 2 min. Title: Line-of-sight velocity in a semiempirical model of a disappearing granule Authors: Koza, J.; Bellot Rubio, L. R.; Kučera, A.; Hanslmeier, A.; Rybák, J.; Wöhl, H. Bibcode: 2002ESASP.506..443K Altcode: 2002svco.conf..443K; 2002ESPM...10..443K The behaviour of the line-of-sight velocity in the centre of a disappearing granule is analyzed using an inversion method applied to a time-series of spectra containing the Fe I 522.5 nm, 557.6 nm and 557.7 nm lines. The temporal evolution of the line-of-sight velocity vLOS is presented in the form of the functional dependence of vLOS(logτ5, t) on the optical depth τ5 at 500 nm and time t. An oscillatory behaviour is found in the velocity stratification with nearly constant phase through the photosphere. The amplitude of variations increases from logτ5 = -0.3 to logτ5 = -2.5 reaching a maximum of ~1.2 km s-1. A zero velocity layer is detected in every instantaneous model of the velocity stratification. The results suggest, that the zero velocity may occur in a considerable range of the optical depths from logτ5 ~ -2 to logτ5 ~ -3.5. Title: Precise reduction of solar spectra obtained with large CCD arrays Authors: Wöhl, H.; Kučera, A.; Rybák, J.; Hanslmeier, A. Bibcode: 2002A&A...394.1077W Altcode: A precise procedure suitable for the reduction of solar spectra taken with large CCD arrays and the retrieval of correct spectral characteristics is presented. Various effects, which one should take into account, are considered and several improvements of the standard reduction are introduced. A special flat-field procedure is suggested for the reduction of spectra registered in different flat-field conditions than those when the flat-field matrix was taken. The original flat-field matrix is split into several components to eliminate the influence of the drift of the spectrograph and temporal changes of the flat-field conditions on the reduced spectrum. The importance of every flat-field matrix component is tested and discussed and the noise propagation through data reduction is analyzed. It is documented that the errors of the basic spectral line characteristics, continuum intensity, line centre intensity and full width at the half maxima of the line have variations between 0.5% and 15% and the errors of the line centre Doppler velocity and bisectors fluctuate by up to 200 m s-1, if derived from imprecise reductions, compared to precise ones. Title: Temporal evolution of physical parameters in granule Authors: Koza, J.; Kucera, A.; Hanslmeier, A.; Rybák, J.; Wöhl, H. Bibcode: 2002ESASP.505..457K Altcode: 2002solm.conf..457K; 2002IAUCo.188..457K The temporal evolution of the physical parameters inside a granule is presented. This is a step towards a more realistic 1D modeling of the solar granulation, avoiding the temporal averaging used up to now. The granulation is treated as a dynamical phenomenon and our model has been calculated using an inversion method applied to time series of spectra. The granular evolutionary model is presented in the form of the functional dependence of temperature T(log τ, t) and line-of-sight velocity vLOS(log τ, t) on optical depth τ and time t. The observed disappearance of the granule is accompanied with significant temperature changes greater than ~300K in deeper layers (log τ5 > 0) and upper layers (log τ5 < -2.5). In contrary, the layers from log τ5 ~= -0.5 to log τ5 ~= -1.5 are more stable in the sense of temperature variations, which are less than ~150K. An oscillatory behavior is found in the line-of-sight velocity stratification from log τ5 ~= 0 upwards with increasing amplitude reaching up to ~= 2 km s-1 in upper layers. Title: Spectral line response to temperature perturbation in solar and stellar photospheric models. I. Neutral Fe I line 522.5nm case Authors: Koza, J.; Kučera, A. Bibcode: 2002CoSka..32..190K Altcode: The sensitivity of the line profile of the neutral Fe I 522.5nm line to Gaussian perturbations of temperature distribution in the photospheric models is examined. Stokes I response functions to temperature of the Fe I 522.5nm line have been calculated using different classes of the solar photospheric models. In the LTE approximation three one-component models HOLMU, HSRA, VAL3C and a new two-component photospheric model are tested. In the (log τ5, λ) plane the response functions have been calculated for all four models. It is shown that in the case of one-component models, the temperature perturbation in the upper photospheric layers only affects the core of the line profile and in contrast, the temperature perturbation of the deep photosphere affects only the line-wings. This is not the case in the two-component model, where the heating or cooling of the upper photosphere significantly modifies not only the line-core but also the wings. A detailed examination of this effect is presented and discussed to point out the incompatibility of simplified one-component models with the real physical conditions of the stellar photosphere. Title: Dynamic coupling of the chromospheric and photospheric flaring plasma Authors: Brceková, K.; Kucera, A.; Hanslmeier, A.; Rybák, J.; Wöhl, H. Bibcode: 2002ESASP.505..357B Altcode: 2002solm.conf..357B; 2002IAUCo.188..357B The relaxing phase of the subflare observed in the core of chromospheric Ca II K line and in two photospheric Fe I 522.5 nm and Fe I 557.6 nm lines was investigated. The temporal evolution of asymmetry in Ca II K line and the mean bisectors positions of the Fe I line profiles as well as their correlations are presented. It is documented that the chromospheric down-flow caused by the subflare strongly affects the upper layers of the photosphere. As a consequence of relaxation of the photospheric layers strong down-flows and up-flows were measured at the end of the subflare relaxing phase. Title: High-resolution CCD spectra reduction: temporal changes of the flat-field compensation Authors: Kučera, Aleš; Hanslmeier, Arnold; Rybák, Ján; Wohl, Hubertus Bibcode: 2002NCimC..25..703K Altcode: A new method suitable for long-time series of high-resolution CCD spectra reduction is presented. The method allows to compensate the temporal changes of the instrument conditions which leads to temporal changes of the flat-field matrix. Sometimes it is impossible to make the flat-field measurements during long simultaneous observations with satellites (SOHO, TRACE). The method splits the flat-field matrix into two components. The first one, connected with CCD camera is stable in time and is correct for all spectra. The second one varies and reflects temporal changes of the conditions in the spectrograph. Description of the method and its application to real high-resolution CCD spectra is presented and discussed. Title: Transition region dynamics from SUMER/SOHO observations: shape of the emission spectral lines Authors: Rybák, J.; Curdt, W.; Kučera, A.; Wöhl, H. Bibcode: 2002ESASP.477..163R Altcode: 2002scsw.conf..163R The quiet sun network/internetwork transition region line profiles of C II 1036.34 Å and O VI 1037.61 Å are outlined emphasizing the temporal/spatial behaviour of their deviations from the Gaussian shape. Systematic deviations of the line profiles from the single-Gaussian shape indicate that transition region emission lines consist of two Gaussian components over almost the whole quiet sun internetwork except their small innermost parts. This finding is in qualitative agreement with the transition region model of Peter (2001). Title: Joint Organization for Solar Observations, Annual Report 2000/2001, Vol. 30/31. Authors: Kucera, A. Bibcode: 2002joso.book.....K Altcode: No abstract at ADS Title: Minutes of the 33rd JOSO Board Meeting - 2001 Authors: Cauzzi, G.; Kucera, A.; Schmieder, B. Bibcode: 2002joso.book...15C Altcode: No abstract at ADS Title: JOSO national report 2000-2001 - Slovakia. Solar research in Slovak Republic 2000-2001 Authors: Kucera, A. Bibcode: 2002joso.book..100K Altcode: Solar research in Slovak Republic is carried out at three following institutions: (1) Astronomical Institute, Slovak Academy of Sciences (AISAS), Tatranská Lomnica (2) Astronomical Institute, Comenius University (AICU), Bratislava (3) Slovak Central Observatory, Hurbanovo. Title: Minutes of the 32nd JOSO Board Meeting - 2000 Authors: Cauzzi, G.; Kucera, A.; Schmieder, B. Bibcode: 2002joso.book...10C Altcode: No abstract at ADS Title: The Location of Solar Oscillations in the Photosphere Authors: Hanslmeier, A.; Kučera, A.; Rybák, J.; Wöhl, H. Bibcode: 2001ASSL..259..267H Altcode: 2001dysu.conf..267H Applying a correlation analysis to time series of granulation it has been shown that due to the influence of enhanced turbulent motions near the downflow regions in the intergranular lanes the turbulent motions predominate. Title: Chromospheric Dynamics as can be Inferred from SUMER/SOHO Observations Authors: Rybák, J.; Kučera, A.; Curdt, W.; Schühle, U.; Wöhl, H. Bibcode: 2001ASSL..259..247R Altcode: 2001dysu.conf..247R Experience with the SUMER/SOHO observations of the chromospheric dynamics and the reduction of the acquired data is summarized on base of the SOHO Joint Operation Program 78 which is focused on the variability of the chromosphere and the transition region to the corona. Title: Dynamics of the Upper Photosphere: Coherence and Phase Analysis (CD-ROM Directory: contribs/hanslmei) Authors: Hanslmeier, A.; Kučera, A.; Rybák, J.; Wöhl, H. Bibcode: 2001ASPC..223..669H Altcode: 2001csss...11..669H No abstract at ADS Title: Correlative relationships in an inhomogeneous solar atmosphere Authors: Gadun, A. S.; Hanslmeier, A.; Kučera, A.; Rybák, J.; Wöhl, H. Bibcode: 2000A&A...363..289G Altcode: We analyse the correlative relationships between various quantities derived from 2-D inhomogeneous and time-dependent model atmospheres and between selected simulated line parameters to compare them with height-dependent correlations derived from spectral observations. We detect three photospheric regions: thermal convection, overshooting convection and a transition layer. We also show that correlations found for the model data and those computed within simulated spectral observations are a good testing tool for line formation depths. As an example, we examine two criteria, providing heights of line core formation in LTE, and conclude that the approach which defines this quantity as geometrical height at line center optical depth τλ0 = 1 is likely more suitable for diagnostic purposes than the method based on depression contribution function. Title: Dynamics of the upper solar photosphere Authors: Hanslmeier, A.; Kučera, A.; Rybák, J.; Neunteufel, B.; Wöhl, H. Bibcode: 2000A&A...356..308H Altcode: The dynamics of the upper solar photosphere was studied by using 1-D photospheric line spectrograms obtained using the VTT of the Observatorio del Teide. Three spectral lines with line core formation heights between 250 and 500 km were analyzed. It is clearly seen that at these levels the velocity and intensity fields are highly correlated but different from the lower lying zone where convective motions predominate. This is shown by classical methods (using correlations and bisectors) as well as by applying the Hurst exponent method to the data. Title: 3-D Tomography of the Solar Photosphere Authors: Hanslmeier, A.; Kucera, A.; Rybak, J.; Wohl, H. Bibcode: 2000ESASP.463..333H Altcode: 2000sctc.proc..333H No abstract at ADS Title: Spectral Statistics of Fe I and Ca II K Lines in the Quiet and Active Solar Atmosphere Authors: Kucera, A.; Brcekova, A. K.; Hanslmeier, A.; Rybak, J.; Woehl, H. Bibcode: 2000HvaOB..24..111K Altcode: Based on two Fe I and Ca II K lines spectra obtained with high spatial and spectral resolution we investigated some spectral characteristics of these lines in quiet and active regions. In this paper we present the behaviour of the central line intensities in different types of solar activity. We discuss the obtained results and compare them with the results reported by other authors. Title: Two Dimensional Spectral Time Series Authors: Hanslmeier, A.; Kucera, A.; Rybak, J.; Woehl, H. Bibcode: 2000HvaOB..24...81H Altcode: We analyze two dimensional time series of solar photospheric spectrograms in order to study the dynamics of solar fine structures and their evolution. The two dimensional images were obtained by scanning over the photosphere. Spectrographic data of this type include a much higher information than ordinary images. Title: Interaction of Sunspots with the Surrounding Plasma - a Progress Report Authors: Woehl, H.; Rybak, J.; Kucera, A. Bibcode: 2000HvaOB..24..119W Altcode: The historic development of the search for interactions of sunspots and solar plasma around them was given in a contribution at the IVth Hvar Astrophysical Colloquium (Woehl, 1997). It was concentrated on the results of measurements and their reductions performed by Lustig and Woehl (1993), showing a dependence of plasma velocity difference in front and behind stable sunspots depending on their relative speed within the plasma. Since the result obtained was not significant, new attempts were started to use MDI/SoHO data and mainly to collect data ourselves at telescopes and the horizontal spectrometer of the Astronomical Institute of the Slovak Academy of Sciences in Tatranska Lomnica, Slovakia. The main difference is that now the plasma velocity data are gained by a matrix of fiber optics collecting light at several positions around the sunspot. In addition the sunspot positions are collected by a different telescope. The reductions of the sunspot positions give very reliable rotation data and - as expected - very small meridional motions, while the plasma velocity data are not yet reliable. Attempts to improve this situation are described. Title: Fe I and Ca II K Lines in Quiet and Active Regions Authors: Kucera, A.; Brcekova, K.; Hanslmeier, A.; Rybak, J.; Wohl, H. Bibcode: 2000ESASP.463..357K Altcode: 2000sctc.proc..357K No abstract at ADS Title: Chromospheric and Transition Region Dynamics - Reasons and Consequences of the Long-period Instrumental Periodicities of SUMER/SOHO Authors: Rybák, J.; Curdt, W.; Kucera, A.; Schühle, U.; Wöhl, H. Bibcode: 1999ESASP.448..361R Altcode: 1999mfsp.conf..361R; 1999ESPM....9..361R No abstract at ADS Title: Chromospheric And Transition Region Dynamics - Reasons and Consequences of the Short Period Instrumental Periodicities of SOHO/SUMER Authors: Rybak, Jan; Curdt, Werner; Kučera, Ales; Schüehle, Udo; Wöehl, Hubertus Bibcode: 1999ESASP.446..579R Altcode: 1999soho....8..579R The instrumentally caused oscillations of the spectral lines intensity and velocity, determined with the SUMER spectrometer onboard SoHO, are presented. On examples of two long-term measurements of O I, C II and O VI lines, it is shown that the reason of this instrumental effect was the insufficient precision of the solar rotation compensation of the spectrometer slit position. In both observational runs the standard rotation compensation procedure, performed on-line by the instrument, was selected for the long-term observations. The minor periodical motion of the slit position on the solar disk was taking place during such observations and this effect produced the regular changes of the measured line intensities and velocities. The significant enhancements of the oscillations amplitudes around the frequency 2.56 mHz and its harmonics were detected in the cases of observations, performed at the disk center. Unfortunately, these frequencies are just in the range of the typical oscillations determined till now in the upper solar atmosphere ! Consequences of this instrumental effect for SUMER measurements of the chromospheric and transition region dynamics are discussed. Procedures how to exclude the effect from the data post-facto as well as how to modify the future SUMER oscillations measurements in order to avoid the effect are proposed Title: Fiber Optics Device for Solar Spectroscopy - First Measurements Authors: Kucera, A.; Rybák, J.; Wöhl, H.; Hanslmeier, A. Bibcode: 1999ASPC..184..319K Altcode: In 1996 we introduced the fiber optics device designed for 2D solar spectroscopy (Kucera et al. 1997). Now we present the first results obtained within last year. First experiences with wavelength calibration, light transmission through the fibers, noise reduction, software for reduction of observations and preliminary results of reduced scientific data are presented. Title: SOHO JOP 078 - variability and properties of the quiet sun supergranular network and internetwork. Authors: Kučera, A.; Curdt, W.; Fludra, A.; Rybák, J.; Wöhl, H. Bibcode: 1999joso.proc..149K Altcode: Study of the variability of the quiet solar atmosphere covering as large as possible range of the temperatures using both the 2D imaging and 1D spectra was the aim of SOHO JOP 78 observations. Supergranular cells were the objects of the authors' main interest. This programme is based on the cooperation of several SOHO instruments (SUMER, CDS, MDI, EIT) and TRACE. Justification of the JOP, cooperation of instruments and specially arranged measurements for the post-facto coalignment of data from different instruments are described in this paper. Title: Correlation of Velocity Fields at Different Heights in the Solar Photosphere Authors: Kucera, A.; Rybák, J.; Wöhl, H. Bibcode: 1999ASSL..239..219K Altcode: 1999msa..proc..219K A simple experimental method for comparison of the line formation heights in the solar photosphere is presented. Several Fe I lines are used to test the method. Title: Heights of formation of FeI photospheric lines Authors: Kucera, A.; Balthasar, H.; Rybak, J.; Woehl, H. Bibcode: 1998A&A...332.1069K Altcode: The determination of the location of spectral line-forming layers by means of line-depression contribution functions is checked by observational tests. The method is based on the assumption that the Doppler velocities derived from line bisectors at a given position in the profile of a spectral line are related to the actual bulk velocity at a particular height in the atmosphere. For a set of six magnetically sensitive and non-sensitive Fe I lines (543.45, 557.61, 630.15, 630.25, 649.50, 649.45 nm) the fluctuations of Doppler velocities along the slit of the spectrograph were determined at various Delta lambda from the line centers i.e. at various heights in the photosphere. Correlations of fluctuations allow us to find those parts in line profiles which are formed at identical heights in the photosphere. These experimental results are compared with theoretical estimates based on line depression contribution functions. The agreement is good and best results are found for nonmagnetic strong, but still unsaturated lines. The results support the hypothesis that it is possible to ascribe a single height point in the solar atmosphere to a given position in a spectral line profile. Title: Oscillations in Chromosphere and Transition Region Based on SUMER Measurements Authors: Kucera, A.; Curdt, W.; Rybák, J.; Schühle, U.; Wöhl, H. Bibcode: 1998ASPC..155..351K Altcode: 1998sasp.conf..351K No abstract at ADS Title: Behaviour of solar active prominence Authors: Kučera, A.; Rybák, J.; Saniga, M. Bibcode: 1998PAICz..88..232K Altcode: No abstract at ADS Title: Measurement of rotational characteristics of sunspots and surrounding photospheric plasma. Authors: Kučera, A.; Rybák, J.; Wöhl, H. Bibcode: 1997joso.proc...68K Altcode: No abstract at ADS Title: Investigation of the Dynamics of Chromosphere and Photosphere from Spectra Obtained by Parallel Observations using SUMER on SOHO and the VTT on Tenerife Authors: Curdt, W.; Kucera, A.; Rybak, J.; Schuhle, U.; Wohl, H. Bibcode: 1997ASPC..118..322C Altcode: 1997fasp.conf..322C This is a preliminary report about parallel observations of chromospheric and photospheric spectra in the ultraviolet and visible spectral regions using SUMER on SOHO and the VTT on Tenerife performed begin of September 1996. The aim is to search for relations of vertical velocity patterns in the upper photosphere and chromosphere in the solar disk center. In addition temporal changes in these parts of the solar atmosphere are investigated. Title: Dynamical Properties of the Chromosphere and Transition Region in the Supergranular Network: What Precision of the Spectral Line Characteristics Can be Reached? Authors: Curdt, W.; Kucera, A.; Rybák, J.; Schühle, U.; Wöhl, H. Bibcode: 1997ESASP.404..307C Altcode: 1997cswn.conf..307C No abstract at ADS Title: Observations of Fe I lines in the quiet solar photosphere. Authors: Kucera, A.; Rybak, J.; Woehl, H. Bibcode: 1995A&A...298..917K Altcode: We investigate three sets of spectra with high spatial and spectral resolution. Each set consists of four spectra taken simultaneously with the Vacuum Tower Telescope at Izana, Tenerife. The main spectral characteristics (continuum intensity I_c_; full width at half maximum FWHM; residual intensity I_o_) were computed for 5 magnetic and non-magnetic Fe I lines (5434.543 A, 5576.099 A, 6301.497 A, 6302.499 A, 6494.994 A). Our results allow a diagnosis of the solar atmosphere in the vertical (two main levels of line formation) and horizontal directions (71 arcseconds). The spectra cover both interior parts of supergranular cells (purely quiet regions, PQR) and cell boundaries (moderate active regions, MAR). The main results are: (1) We find a different continuum intensity distribution for PQRs and MARs, which reflects the existence of different patterns in these regions. The difference is also evident in the rms residual intensity fluctuation. (2) A significant minimum of the residual intensity fluctuations (δI_o_/I_c_)_rms_ occurs at a height of about 300km. (3) At all heights of the PQRs the line widths FWHM in the intergranular lanes are larger than the mean line width; those in the granules are smaller. This variation of the FWHM is influenced by a magnetic effect near the centres of the intergranular lanes (reduced FWHM), and by the effect of convection in granules (enhanced FWHM). (4) The correlation <I_c_, I_o_> reverses its sign at a height of about 250km. The anticorrelation in the range 300-500km indicates a non-convective structure, different from the photospheric granular pattern found earlier. Title: Contributions of the Astronomical Observatory Skalnate Pleso, Volume 25 Authors: Zverko, Juraj; Antalova, Anna; Svoren, Jan; Chochol, Drahomir; Kucera, Ales; Porubcan, Vladimir Bibcode: 1995STIN...9624442Z Altcode: Topics addressed include astrometry of minor planets, solar magnetic sectors and spatial distribution of LDE-type flares, radar observations of the Perseid meteor shower, periodic variations in the light curves of symbiotic stars, photometry of symbiotic stars, even-odd solar-cycle differences of corona brightness, solar eclipses, and index of cosmic ray fluctuations at neutron monitor energies. Also addressed is stratification of chromium abundance in CP-stars alpha2 Canum Venaticorum, epsilon Ursae Majoris, Sirius and Vega. Title: A Solar Plage Model Authors: Kucera, A.; Baranovsky, E. A. Bibcode: 1994IAUS..154...29K Altcode: No abstract at ADS Title: JOSO Workshop: Instrumentation for magnetic field measurements Authors: Kucera, A. Bibcode: 1994imfm.conf.....K Altcode: No abstract at ADS Title: Mass Ejections from Chromosphere to Corona: Results from a Spectral Analysis Authors: Kučera, A.; Rybák, J.; Minaroviech, M. Bibcode: 1994emsp.conf..147K Altcode: No abstract at ADS Title: Magnetic and nonmagnetic line profiles in solar quiet and active regions Authors: Kučera, A.; Rybák, J.; Wöhl, H. Bibcode: 1994smf..conf..291K Altcode: No abstract at ADS Title: H-Alpha Morphology of Gamma-Flares Authors: Kucera, A.; Antalová, A. Bibcode: 1994step.conf..151K Altcode: No abstract at ADS Title: Joint Organization for Solar Observations (24th meeting). Authors: Kucera, A. Bibcode: 1993Kozmo..24...23K Altcode: No abstract at ADS Title: Hot mass transport in the solar active prominence Authors: Kucera, A.; Saniga, M.; Rybak, J. Bibcode: 1992AIPC..267..160K Altcode: 1992ecsa.work..160K On October 16, 1990, a remarkable active prominence was observed, in Hα line, during 113 minutes. The time gap between successive profile recordings was 20 seconds and 339 profiles have been recorded together. We focused our attention on Doppler shift measurements as well as on significant changes in the prominence intensity. We also give a possible explanation of a sudden increment in the intensity of Hα line in dependence on the fact if the whole profile originates in one particular place in the prominence or if it is a superposition of the radiation incident from two different, physically unrelated parts of the prominence. Title: Height-Dependent Solar Plage Temperature Distribution (With 3 Figures) Authors: Kucera, A.; Scherbakova, Z.; Baranovsky, E. Bibcode: 1991mcch.conf..109K Altcode: No abstract at ADS Title: The horizontal solar telescope with spectrograph at Stará Lesná Observatory Authors: Kucera, A.; Rybak, J.; Minarovjech, M.; Novocky, D.; Saniga, M. Bibcode: 1990Ap&SS.171..279K Altcode: The construction and the optical design as well as the controlling electronic device and the spectrum recording of the new horizontal solar telescope with the spectrograph of the Astronomical Institute of Slovak Academy of Sciences are described. Also some of its adjustments and improvements are briefly mentioned. Title: The H, K and IR triplet of Ca II in plages. Authors: Baranovskij, Eh. A.; Kuchera, A.; Kučera, A.; Shcherbakova, Z. A. Bibcode: 1987IzKry..77....3B Altcode: The observed profiles of Ca II lines H, K, λ8498, λ8542, λ8662 are obtained and the model chromospheres are derived for plages of different brightness. The calculations involve the program of non-LTE spectra analysis. The density in the bright plages is of an order of 2 higher than that of the undisturbed chromosphere. The models of weak plages do not differ significantly from the undisturbed model chromosphere. Title: Can small-scale bipolar structures originate in the solar atmosphere ? Authors: Saniga, M.; Kučera, A.; Novocký, D.; Rybák, J. Bibcode: 1986CoSka..15..683S Altcode: Using the formalism of the magnetohydrodynamics shock waves the simple model of the origin of small-scale bipolar structures in a magnetized plasma is outlined. It is shown that there are regions in the atmosphere of the Sun where such object can naturally occur. Properties of these structures and their typical dimension are examined. Title: Relationships of a growing magnetic flux region to flares Authors: Martin, S. F.; Bentley, R. D.; Schadee, A.; Antalova, A.; Kucera, A.; Dezső, L.; Gesztelyi, L.; Harvey, K. L.; Jones, H.; Livi, S. H. B.; Wang, J. Bibcode: 1984AdSpR...4g..61M Altcode: 1984AdSpR...4...61M Some sites for solar flares are known to develop where new magnetic flux emerges and becomes abutted against opposite polarity pre-existing magnetic flux (review by Galzauskas/1/). We have identified and analyzed the evolution of such flare sites at the boundaries of a major new and growing magnetic flux region within a complex of active regions, Hale No. 16918. This analysis was done as a part of a continuing study of the circumstances associated with flares in Hale Region 16918, which was designated as an FBS target during the interval 18 - 23 June 1980. We studied the initiation and development of both major and minor flares in Hα images in relation to the identified potential flare sites at the boundaries of the growing flux region and to the general development of the new flux. This study lead to our recognition of a spectrum of possible relationships of growing flux regions to flares as follows: (1) intimate interaction with adjacent old flux - flare sites centered at new/old flux boundary, (2) forced or ``intimidated'' interaction in which new flux pushes old field having lower flux density towards a neighboring old polarity inversion line where a flare then takes place, (3) ``influential'' interaction - magnetic lines of force over an old polarity inversion line, typically containing a filament, reconnect to the new emerging flux; a flare occurs with erupting filament when the magnetic field overlying the filament becomes too weak to prevent its eruption, (4) inconsequential interaction - new flux region is too small or has wrong orientation for creating flare conditions, (5) incidental - flare occurs without any significant relationship to new flux regions. Title: The Crimean Astrophysical Observatory. Authors: Kučera, A. Bibcode: 1984Kozmo..15...10K Altcode: No abstract at ADS Title: Irregular Rotation of the Main Sunspot in Active Region Hale 17 570 of 5-13 April 1981 Authors: Kucera, A. Bibcode: 1982BAICz..33..345K Altcode: No abstract at ADS Title: Emerging magnetic flux, flares and filaments - FBS interval 16-23 June 1980 Authors: Martin, S. F.; Dezso, L.; Antalova, A.; Kucera, A.; Harvey, K. L. Bibcode: 1982AdSpR...2k..39M Altcode: 1982AdSpR...2...39M 17 emerging magnetic flux regions with arch filaments related to new sunspots were identified in Hale Active Region No. 16918 during the 7 day interval from 16-22 June. Most of the new flux regions were clustered around the filament channel between the old opposite polarity fields as were most of the flares. The two largest regions of new magnetic flux and a few of the smaller flux regions developed very near the end points of filaments. This suggests that the emergence of flux in existing active regions might be non-random in position along a filament channel as well as in distance from a filament channel.

We have analyzed the positions of 88 flares to date during about half of each day. We find that slightly more than half (50%) of the flares, irrespective of their size, are centered within the new flux regions. About 1/5 (20%) were centered on the border between the new flux and the adjacent older magnetic field. Less than 1/3 occurred outside of the newly emerging flux regions but in many cases were very close to the newly emerging flux. We conclude that at least 2/3 of the flares are intimately related to the emerging flux regions while the remaining 1/3 might be either indirectly related or unrelated to the emerging flux. Title: Search for the Period of the Binary Shell Star V505 Monocerotis Authors: Chochol, D.; Kucera, A. Bibcode: 1981IBVS.1998....1C Altcode: No abstract at ADS