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Author name code: kucera-ales
ADS astronomy entries on 2022-09-14
author:"Kucera, Ales"

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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
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.

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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.
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<SUP>-1</SUP> next
  to the pores and to 4 km s<SUP>-1</SUP> 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.

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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.
2017A&A...602A..60G    Altcode: 2017arXiv170406089G
  <BR /> 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. <BR /> 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). <BR /> 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. <BR /> 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. <P
  />The movie associated to Figs. 4 and 5 is available at <A
  href="http://www.aanda.org/10.1051/0004-6361/201730644/olm">http://www.aanda.org</A>

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Title: Propagation of filament and hot plasma through solar atmosphere
    as observed with ground based and space instruments
Authors: Kucera, A.
2017psio.confE..73K    Altcode:
  No abstract at ADS

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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.
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.

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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.
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<SUP>-1</SUP> 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.

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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.
2016ASPC..504..205S    Altcode:
  An active region mini-filament was observed by VTT simultaneously
  in the He&lt;small&gt;I&lt;/small&gt; 10 830 Å triplet by the TIP 1
  spectropolarimeter, in Hα by the TESOS Fabry-Pérot interferometer, and
  in Ca &lt;small&gt;II&lt;/small&gt; 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.

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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.
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.

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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
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.

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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
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.

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Title: Inferring spectral characteristics of the Hα spectral line
    observed by the DOT Lyot filter
Authors: Koza, J.; Rybák, J.; Gömöry, P.; Kučera, A.
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 4<SUP>th</SUP>-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<SUP>-1</SUP>. When using the 4<SUP>th</SUP>-order
  polynomial, deviations are within the interval ±2.5 km s<SUP>-1</SUP>,
  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.

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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.
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.

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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.
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.

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Title: Search for Alfvén waves in a bright network element observed
    in Hα
Authors: Koza, J.; Sütterlin, P.; Gömöry, P.; Rybák, J.;
   Kučera, A.
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
  4<SUP>th</SUP>-order polynomial. The bright network element displays
  the most pronounced variations of the Dopplershift varying from 0 to 4
  km s<SUP>-1</SUP> about the average of 1.5 km s<SUP>-1</SUP>. This fact
  implies a persistent redshift of the Hα core with a redward asymmetry
  of about 0.5 km s<SUP>-1</SUP>, 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.

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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.
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<SUP>-1</SUP> the error is below 1 %.

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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.
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].

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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.
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.

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Title: Koronálny multikanálový polarimeter pre observatórium
Lomnický štít 

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Title: Koronálny multikanálový polarimeter
pre observatórium Lomnický štít 

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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.
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.
2010A&A...511A..14G    Altcode: 2009arXiv0910.4449G
  <BR /> Aims: We investigate the temporal evolution of magnetic
  flux emerging within a granule in the quiet-Sun internetwork at
  disk center. <BR /> 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. <BR /> 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 × 10<SUP>17</SUP> 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. <BR />
  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
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 ( I<SUB>N</SUB>), the length of magnetic shear of the
  main neutral line ( L<SUB>ss</SUB>), the flux normalized measure of
  the field twist (α={μI<SUB>N</SUB>}/{Φ}) with μ being the magnetic
  permeability. The current helicity ( H<SUB>c</SUB>) 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.
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.
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. <P />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. <P />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. <P />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.
2008ESPM...12.2.52K    Altcode:
  Spatial and temporal evolution of dynamic fibrils (DF) as well as
  coupling with photospheric features was investigated. <P />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. <P />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.
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.
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<SUP>-1</SUP> 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.
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.
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.
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. <P />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.
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.
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. <P />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. <P />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.
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.<BR /> 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.<BR /> 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.<BR />

---------------------------------------------------------
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
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.
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
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.
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.
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.
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.
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.
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
  <P />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.
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.
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.
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.
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.
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.
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.
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.
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.
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.
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.
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.
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(logτ<SUB>5</SUB>,t)
  and (t) on the continuum optical depth τ<SUB>5</SUB> at 500 nm and
  time t. A ľof several hundreds of meters per second was found in the
  upper photosphere (logτ<SUB>5</SUB>≤-1.5), where the plasma flows
  away from the observer. On the contrary, upflows directed toward the
  observer were found in deeper layers (logτ<SUB>5</SUB>&gt;-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.
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.
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.
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.
2003CoSka..33..224K    Altcode:
  Stokes I response functions to the line-of-sight velocity
  v<SUB>LOS</SUB> 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 v<SUB>LOS</SUB> is examined and
  the range of reliability of v<SUB>LOS</SUB> 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 v<SUB>LOS</SUB>. In
  the case of the Fe I 522.5 nm line the impact of a v<SUB>LOS</SUB>
  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.
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.
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.
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.
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 &gt;=0) and upper layers
  (log tau_5 &lt;=-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 &lt;=-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.
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.
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<SUP>-1</SUP>. 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.
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
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.
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 v<SUB>LOS</SUB> is presented in the form of the functional
  dependence of v<SUB>LOS</SUB>(logτ<SUB>5</SUB>, t) on the optical
  depth τ<SUB>5</SUB> 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
  logτ<SUB>5</SUB> = -0.3 to logτ<SUB>5</SUB> = -2.5 reaching a maximum
  of ~1.2 km s<SUP>-1</SUP>. 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 logτ<SUB>5</SUB> ~ -2 to logτ<SUB>5</SUB> ~ -3.5.

---------------------------------------------------------
Title: Precise reduction of solar spectra obtained with large
    CCD arrays
Authors: Wöhl, H.; Kučera, A.; Rybák, J.; Hanslmeier, A.
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<SUP>-1</SUP>, 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.
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 v<SUB>LOS</SUB>(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 τ<SUB>5</SUB> &gt; 0) and upper layers (log τ<SUB>5</SUB> &lt;
  -2.5). In contrary, the layers from log τ<SUB>5</SUB> ~= -0.5 to log
  τ<SUB>5</SUB> ~= -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<SUP>-1</SUP>
  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.
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 τ<SUB>5</SUB>, 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.
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
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.
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.
2002joso.book.....K    Altcode:
  No abstract at ADS

---------------------------------------------------------
Title: Minutes of the 33rd JOSO Board Meeting - 2001
Authors: Cauzzi, G.; Kucera, A.; Schmieder, B.
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.
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.
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.
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.
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.
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.
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
  τ<SUB>λ0</SUB> = 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.
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.
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.
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.
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.
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.
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.
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
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.
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.
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.
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.
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.
1998ASPC..155..351K    Altcode: 1998sasp.conf..351K
  No abstract at ADS

---------------------------------------------------------
Title: Behaviour of solar active prominence
Authors: Kučera, A.; Rybák, J.; Saniga, M.
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.
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.
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.
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.
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 &lt;I_c_, I_o_&gt; 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
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 alpha<SUP>2</SUP>
  Canum Venaticorum, epsilon Ursae Majoris, Sirius and Vega.

---------------------------------------------------------
Title: A Solar Plage Model
Authors: Kucera, A.; Baranovsky, E. A.
1994IAUS..154...29K    Altcode:
  No abstract at ADS

---------------------------------------------------------
Title: JOSO Workshop: Instrumentation for magnetic field measurements
Authors: Kucera, A.
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.
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.
1994smf..conf..291K    Altcode:
  No abstract at ADS

---------------------------------------------------------
Title: H-Alpha Morphology of Gamma-Flares
Authors: Kucera, A.; Antalová, A.
1994step.conf..151K    Altcode:
  No abstract at ADS

---------------------------------------------------------
Title: Joint Organization for Solar Observations (24th meeting).
Authors: Kucera, A.
1993Kozmo..24...23K    Altcode:
  No abstract at ADS

---------------------------------------------------------
Title: Hot mass transport in the solar active prominence
Authors: Kucera, A.; Saniga, M.; Rybak, J.
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.
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.
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.
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.
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.
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.
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.
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.
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. <P
  />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.
1981IBVS.1998....1C    Altcode:
  No abstract at ADS