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Author name code: svestka
ADS astronomy entries on 2022-09-14
author:"Svestka, Zdenek" 

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Title: Sixty Years in Solar Physics
Authors: Švestka, Zdeněk
2010SoPh..267..235S    Altcode: 2010SoPh..tmp..235S; 2010SoPh..tmp..211S
  I recount my career in solar physics beginning at Ondřejov Observatory
  in 1948 and ending with my ∼30 year stay at the Laboratory of Space
  Research in Utrecht.

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Title: The Misnomer of “Post-Flare Loops”
Authors: Švestka, Zdeněk
2007SoPh..246..393S    Altcode:
  Attention is drawn to the fact that the term "post-flare loops" is
  incorrect and should be avoided, because the loops are parts of the
  flare itself. Two other names for these loop systems are suggested.

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Title: Editorial Appreciation
Authors: Engvold, Oddbjørn; Harvey, Jack; Leibacher, John; Sakurai,
   Takashi; Švestka, Zdeněk; van Driel-Gesztelyi, Lidia; Solar Physics
   editors
2006SoPh..233....1E    Altcode:
  No abstract at ADS

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Title: Preface
Authors: Rottman, G.; Woods, T.; George, V.; Harvey, J.; Švestka,
   Z.; Engvold, O.
2005SoPh..230....1R    Altcode:
  No abstract at ADS

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Title: Evidence Linking Slow Solar Wind Streams to Long-Decay
    X-Ray Events
Authors: Švestka, Zdeněk; Fárník, František
2005SoPh..229..305S    Altcode:
  Outflow of slow solar wind from solar active regions has been reported
  in recent years by many different authors. Therefore, in this paper
  we have studied synoptic maps of the solar wind density (SWD) based
  on interplanetary scintillation (IPS) data for available parts of all
  the years 1991-1994 and 1997-2001 to verify correlations of maxima in
  SWD with sources in active regions. We have found convincing evidence
  that eruptive flares in active regions, and thus X-ray long-decay
  events (LDEs) in general, can produce short-lived enhancements of
  the SWD. However, we were not able to get statistically convincing
  evidence that active regions can be permanent sources of slow solar
  wind, and propose three possible reasons for this negative result.

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Title: Editorial
Authors: Engvold, Oddbjorn; Harvey, Jack; Švestka, Zdenek
2005SoPh..229....1E    Altcode:
  No abstract at ADS

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Title: Hard x-ray Pulsations in the Initial Phase of Flares
Authors: Fárník, F.; Karlický, M.; Švestka, Z.
2003SoPh..218..183F    Altcode:
  When analyzing light curves of hard X-ray bursts recorded by the Hard
  X-Ray Spectrometer on board the MTI satellite, we have found three
  events (all associated with major solar flares, two of them in the same
  active region) which show pulsations in the very initial phase of the
  burst. Periods of the pulsations range from 25 to 48 s. We compare them
  with other observations of pulsations of radio waves and in X-rays
  and conclude that pulsations of this kind have not been observed
  before. We mention several possible causes and prefer interactions
  between current-carrying loops as the most likely interpretation of
  the observed variations.

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Title: Solar activity
Authors: Švestka, Z.
2003dysu.book..237S    Altcode:
  What is the active Sun which is a very important factor in our
  life? Observations from SOHO and TRACE reveal the highly turbulent
  nature of Sun's surface and its atmospheric layers: all the time and
  everywhere we see brightness variations, loop formations and decays,
  plasma flows and ejections of gas. However, this is not what we call
  solar activity. The real processes called solar activity appear only
  in limited parts of the solar surface, and their occurrence varies
  quasi-periodically with time, creating 11-year cycles of solar activity
  whose main characteristics are described in this chapter. Particular
  attention is paid to coronal mass ejections, as the most important
  phenomenon affecting the Earth.

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Title: Preface
Authors: Lin, R.; Dennis, B.; Benz, A.; Harvey, J.; Engvold, O.;
   švestka, Z.
2002SoPh..210....1L    Altcode:
  No abstract at ADS

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Title: X-ray Jets in Interconnecting Loops
Authors: Fárník, František; Švestka, Zdeněk.
2002SoPh..206..143F    Altcode:
  We present examples of X-ray jets, observed by the Soft X-ray Telescope
  on board Yohkoh, which followed trajectories of transequatorial
  interconnecting loops (TILs). All these TILs were preexisting, seen
  some time before, but were mostly invisible at the time of the onset
  of the jet which often made them bright along their total length. With
  few exceptions, these TIL-associated jets have properties very similar
  to other jets ejected inside active regions or along open field lines
  (footpoints in X-ray bright points, recurrence, strong collimation,
  average speed close to 350 km s<SUP>−1</SUP>), but may reach larger
  lengths, in our examples up to 450 000 km. Exceptions are one jet that
  moved slower and one that had no brightened area at its supposed source
  region at the time of its origin (an X-ray bright point appeared there
  only 3 hours later). It appears that quite a high number of X-ray jets
  may be of this TIL-associated kind.

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Title: Flare Changes Associated with Peaks of Hard X-Ray Bursts
Authors: Farnik, F.; Svestka, Z.; Karlicky, M.
2002cosp...34E1403F    Altcode: 2002cosp.meetE1403F
  Using the high-resolution records made in four energy channels
  by the Hard X-Ray Spectrometer (HXRS) on board the MTI spacecraft
  (launched on 12 March 2000) we try to refine the study made by Dwivedi
  et al. 18 years ago (Dwivedi, B.N., Hudson, H.S., Kane, S.R., and
  Svestka, Z.: 1984, Solar Phys. 90, 331) who looked for changes in the
  flare development associated with changes in the hard X-ray flux. In
  addition to H-alpha and SOHO data we can, at least for some flares,
  also use high-resolution TRACE images which make it possible to see
  fine changes which could not be detected before. We try to find, in
  particular, which parts of flares produce hard X ray peaks of various
  hardness in the HXRS records and we also- compare them with peaks in
  microwave records. Intense peaks often correspond to flaring structures
  penetrating into strong magnetic fields (penumbrae and umbrae of
  sunspots) which generally confirms Dwivedi et al.'s findings. However,
  we can provide more details than they were able to obtain from their
  data with worse space and time resolution.

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Title: X-Ray Jets in Interconnecting Loops
Authors: Fárník, F.; Švestka, Z.
2002mwoc.conf...81F    Altcode:
  We present several examples of X-ray jets, observed by the SXT onboard
  Yohkoh, which followed trajectories of transequatorial interconnecting
  loops (TILs). All these TILs were preexisting, seen some time before,
  but mostly invisible at the time of the onset of the jet which often
  made them bright along their total length. With few exceptions, these
  TIL-associated jets have properties very similar to other jets ejected
  inside active regions or along open field lines (footpoints in X-ray
  bright points, recurrence, strong collimation, average speed between
  340 and 380 km s-1, but may reach very large lengths, in excess of
  450 000 km. Exceptions are one jet that moved slower and one that
  had no brightened area at its source region at the time of its origin
  (an X-ray bright point appeared there only 3 hours later). It appears
  that less than 20% of X-ray jets are of this kind.

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Title: Locations of Footpoints of Transequatorial Interconnecting
    Loops
Authors: Fárník, František; Karlický, Marian; Švestka, Zdeněk.
2001SoPh..202...81F    Altcode:
  We discuss footpoints of loops seen by Yohkoh in soft X-rays
  that connect active regions across the equator (transequatorial
  interconnecting loops - TILs). While most TILs are rooted in moderately
  strong fields at peripheries of active regions, there are also cases
  when these loops are anchored in very weak or very strong fields,
  ranging from &lt; 30 G to several hundred gauss. Some have their
  footpoints near sunspot penumbrae, creating `X-ray fountains' in a
  combination with active region loops. But TILs are never rooted in
  sunspots. The most likely explanation is that magnetic field lines
  leave spots almost vertically so that TILs rooted in them extend high
  into the corona and density in them is below the limit of visibility
  in X-rays. The fact that in force-free modeling some TILs are rooted
  in sunspots is most probably due to the difference between field-line
  connections in `vacuum' and in the highly conductive plasma on the
  Sun. Some TILs end before they reach active regions which sometimes
  may indicate the real situation, but mostly this `gap' is probably due
  to a temperature decrease near the loop footpoints which makes them
  invisible in X-rays. In that case the fact that these cool lowest parts
  of TILs are never found in TRACE or SOHO EIT images indicates that
  plasma density in TILs must be very low. Still, the total absence of
  any counterparts of X-ray TILs in TRACE and EIT images is puzzling and,
  therefore, other possible interpretations of the `gap' origin are also
  briefly mentioned.

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Title: Varieties of Coronal Mass Ejections and Their Relation
    to Flares
Authors: Švestka, Zdeněk.
2001SSRv...95..135S    Altcode:
  Most coronal mass ejections (CMEs) start as coronal storms which are
  caused by an opening of channels of closed field lines along the zero
  line of the longitudinal magnetic field. This can happen along any
  zero line on the Sun where the configuration is destabilized. If
  the opening includes a zero line inside an active region, one
  observes a chromospheric flare. If this does not happen, no flare
  is associated with the CME in the chromosphere, but the process,
  as well as the response in the corona (a Long Decay Event in X-rays)
  remains the same. The only difference between flare-associated and
  non-flare-associated CMEs is the strength of the magnetic field in
  the region of the field line opening. This can explain essentially
  all differences which have been observed between these two kinds
  of CMEs. However, there are obviously also other sources of CMEs,
  different from coronal storms: sprays (giving rise to narrow, pointed
  ejections), erupting interconnecting loops (often destabilized by
  flares), and growing coronal holes. This paper tries to summarize
  and interpret observations which support this general picture, and
  demonstrates that both CMEs and flares must be properly discussed in
  any study of solar-terrestrial relations.

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Title: Solar Flares: Main Phase
Authors: Švestka, Z.
2000eaa..bookE2290S    Altcode:
  After the impulsive phase of a flare is over (see SOLAR FLARES:
  IMPULSIVE PHASE), we talk about the main phase or gradual phase. Most
  FLARES (often called compact or confined flares) are short lived
  and they simply cool during the main phase, decaying within minutes
  or tens of minutes. However, there is also another kind of flares
  (eruptive flares) which continue to release energy during their ma...

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Title: Helioseismic Diagnostics of Solar Convection and Activity
Authors: Svestka, Zdenek; Harvey, John W.
2000hdsc.conf.....S    Altcode:
  This book focuses on the recent advances in our understanding of
  solar convection and activity, and on new methods and results of
  helioseismic diagnostics of the internal structures and dynamics
  of solar convection and active regions. The methods of local
  helioseismology (time-distance tomography, ring-diagram analysis,
  acoustic imaging, and holography) intensively developed in the past
  few years have provided promising results on the deep structure
  of large-scale convection and flows, emerging active regions, and
  sunspots. The book includes reviews and contributed papers presented at
  the SOHO-9 Workshop held on July 12-15, 1999, at Stanford University,
  California, U.S.A. It provides a comprehensive overview of the
  current status of the field and presents new ideas and approaches
  to helioseismic diagnostics and theoretical modeling of the physical
  processes inside the Sun. The book is recommended for graduate students
  and specialists in solar physics, astrophysics, and geophysics. Link:
  http://www.wkap.nl/book.htm/0-7923-6520-8

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Title: Helioseismic diagnostics of solar convection and activity. Part
    1, 2. Proceedings. SOHO-9 Workshop, Stanford, CA (USA), 12 - 15
    Jul 1999.
Authors: Švestka, Z.; Harvey, J. W.; Kosovichev, A. G.; Duvall,
   T. L., Jr.
2000SoPh..192....1S    Altcode:
  The following topics were dealt with: theories of solar convection,
  rotation and activity, helioseismic tomography, acoustic imaging and
  holography, ring-diagram analysis, magnetic fields and oscillations,
  solar cycle variations of the internal structure and rotation, solar
  convective structures and oscillations.

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Title: Solar activity: An overview
Authors: Švestka, Zdenek
1999CSci...77.1503S    Altcode:
  No abstract at ADS

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Title: G. Burkhardt, U. Esser, H. Hefele, I. Heinrich, W. Hofmann,
    V. R. Matas, L. D. Schmadel, R. Wielen, and G. Zech (eds.), Astronomy
    and Astrophysics Abstracts, Volumes 69A and 69B
Authors: Švestka, Z.
1999SoPh..188..217S    Altcode:
  No abstract at ADS

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Title: Quiet solar wind signatures above active regions observed
    in X-rays
Authors: Hick, P.; Svestka, Z.; Jackson, B. V.; Farnik, F.; Hudson, H.
1999AIPC..471..231H    Altcode: 1999sowi.conf..231H
  X-ray images from the Yohkoh satellite, obtained following occurrences
  of limb flares sometimes show coronal fan-like structures extending
  above a growing post-flare loop system. We show one such event
  observed in AR 7270 on the east limb of the Sun on 28/29 August
  1992. We suggest that these rays are `ministreamers,' formed as a
  result of the re-structuring of the corona following the occurrence
  of a flare-associated CME. Synoptic maps of the solar wind density,
  constructed from a tomographic analysis of interplanetary scintillation
  (IPS) measurements, show enhanced scintillation matching the position
  of AR 7270 if we assume a radial outflow at a reasonable slow solar
  wind speed of 400 km s-1. From this agreement we argue that outflow
  of mass occurs from the active region into interplanetary space.

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Title: Long transequatorial interconnecting loops of the new solar
    cycle
Authors: Fárník, F.; Karlický, M.; Švestka, Z.
1999SoPh..187...33F    Altcode:
  We study two long transequatorial loops connecting high-latitude
  regions of the new solar cycle. These loops (with lengths of 47 and
  61 heliographic degrees) provide evidence that the upper length limit
  of 37° found by Chase et al. (1976) from Skylab data was determined
  simply by the typical distances between northern and southern active
  regions during the period of Skylab observations. We find strong
  support for the idea that these long interconnecting loops originate
  through reconnection of field lines extending from the two active
  regions towards and beyond the equator, and confirm the earlier
  finding by Canfield, Pevtsov, and McClymont (1996) that only field
  lines from active regions with the same chirality reconnect. As we
  are not aware of any longitudinal (E-W) loops of comparable lengths,
  we suggest that it is mainly the solar differential rotation which
  drives the reconnection of latitudinal (N-S) field lines.

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Title: The Gradual Phase of Flares
Authors: Svestka, Z. F.; Poletto, G.; Fontenla, J.; Hick, P.; Kopp,
   R. A.; Sylwester, B.; Sylwester, J.
1999mfs..conf..409S    Altcode:
  Heating and Cooling in the Gradual Phase Emission Measure-Temperature
  Diagrams Flaring Arches Gradual Phase of Eruptive Flares Postflare
  Giant Arches Giant Arches: Modeling and Interpretation

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Title: Large-Scale Active Coronal Phenomena in Yohkoh SXT Images
    IV. Solar Wind Streams from Flaring Active Regions
Authors: Švestka, Zdeněk; Fárník, František; Hudson, Hugh S.;
   Hick, Paul
1998SoPh..182..179S    Altcode:
  We demonstrate limb events on the Sun in which growing flare loop
  systems are embedded in hot coronal structures looking in soft X-rays
  like fans of coronal rays. These structures are formed during the flare
  and extend high into the corona. We analyze one of these events, on
  28-29 August 1992, which occurred in AR 7270 on the eastern limb, and
  interpret these fans of rays either as temporary multiple ministreamers
  or plume-like structures formed as a result of restructuring due to
  a CME. We suggest that this configuration reflects mass flow from the
  active region into interplanetary space. This suggestion is supported
  by synoptic maps of solar wind sources constructed from scintillation
  measurements which show a source of enhanced solar wind density at
  the position of AR 7270, which disappears when 5 days following the
  event are removed from the synoptic map data. We also check synoptic
  maps for two other active regions in which existence of these fan-like
  structures was indicated when the active regions crossed both the east
  and west limbs of the Sun, and both these regions appear to be sources
  of a density enhancement in the solar wind.

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Title: Fan-Like coronal X-ray Structures as Sources of Solar Wind
Authors: Hick, P.; Svestka, Z.; Farnik, F.; Hudson, H. S.; Jackson,
   B. V.
1998AAS...192.1503H    Altcode: 1998BAAS...30..840H
  We show coronal soft X-ray images from the Yohkoh satellite, obtained
  following occurrences of limb flares. These images show rising
  post-flare loops, which are embedded in hot coronal structures looking
  like fans of coronal rays. We analyze the event on 28/29 August 1992,
  which occurred in AR 7270 on the east limb of the Sun. We suggest that
  these rays are multiple 'ministreamers', which apparently are formed as
  a result of the restructuring of the corona following the occurrence
  of a flare-associated CME. We argue that this configuration allows
  outflow of mass from the active region into interplanetary space. This
  is supported by synoptic maps of solar wind sources constructed from
  scintillation measurements showing a source of enhanced scintillation
  at the position of AR 7270.

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Title: Post-Flare Structures Rising with Decreasing or Constant Speed
Authors: Svestka, Z.; Farnik, F.
1998ASSL..229..365S    Altcode: 1998opaf.conf..365S
  No abstract at ADS

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Title: A Window to the West
Authors: Svestka, Zdenek
1998fyc..conf...75S    Altcode:
  No abstract at ADS

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Title: Large-Scale Active Coronal Phenomena in YOHKOH SXT
    Images. III. Enhanced Post-Flare Streamer
Authors: Švestka, Zdeněk; Fárník, František; Hick, Paul; Hudson,
   Hugh S.; Uchida, Yutaka
1997SoPh..176..355S    Altcode:
  We demonstrate several events where an eruptive flare close to the
  limb gave rise to a transient coronal streamer visible in X-rays in
  Yohkoh SXT images, and analyze one of these events, on 28-29 October
  1992, in detail. A coronal helmet streamer began to appear 2 hours
  after the flare, high above rising post-flare loops; the streamer
  became progressively narrower, reaching its minimum width 7-12 hours
  after the flare, and widened again thereafter, until it eventually
  disappeared. Several other events behaved in a similar way. We suggest
  that the minimum width indicates the time when the streamer became
  fully developed. All the time the temperature in the helmet streamer
  structure was decreasing, which can explain the subsequent fictitious
  widening of the X-ray streamer. It is suggested that we may see here
  two systems of reconnection on widely different altitudes, one giving
  rise to the post-flare loops while the other creates (or re-forms)
  the coronal helmet streamer. A similar interpretation was suggested in
  1990 by Kopp and Polettofor post-flare giant arches observed on board
  the SMM; indeed, there are some similarities between these post-flare
  helmet streamers and giant arches and, with the low spatial resolution
  of SMM instruments, it is possible that some helmet streamers could
  have been considered to be a kind of a giant arch.

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Title: Solar Physics Announces CD-ROM
Authors: Svestka, Zdenek; Howard, Robert F.; Engvold, Oddbjorn
1997SoPh..176..443S    Altcode:
  No abstract at ADS

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Title: Post-Flare Loops Embedded in a Hot Coronal Fan-Like Structure
Authors: Švestka, Z.; Fárnik; Hudson, H. S.; Hick, P.
1997ESASP.415..139S    Altcode: 1997cpsh.conf..139S
  No abstract at ADS

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Title: Observations of Faint, Outlying Loop Systems in Large Flares
Authors: Neidig, Donald F.; Švestka, Zdeněk; Cliver, Edward W.;
   Airapetian, Vladimir; Henry, Timothy W.
1997SoPh..170..321N    Altcode:
  Faintly visible, darkened regions in Hα lying outside but
  adjacentto bright flare emissionwere found to occur in 10 of 31 major
  flares investigated. Without exception, the darkenings occur over
  `magnetically neutral' areas, and these are usually bordered by ridges
  ofoppositely-poled field, where one border is shared in common with a
  flare ribbon. Thedarkenings probably result from the formation of faint,
  outlying loop systems, similar topost-flare loops seen in absorption,
  but which are connected to magnetic features outsidethe flare and
  are unresolved or only marginally resolved in patrol images. Simple
  modelsfor post-flare loops incorporating the results of statistical
  equilibrium calculations readilydemonstrate that darkenings of several
  percent (consistent with our photometric measurements) can be produced
  by loop structures of cross-sectional diameter ≈ 10<SUP>2</SUP> km
  (unresolved by patrol instruments) and containing gas at densities 5 ×
  10<SUP>10</SUP>-5 × 10<SUP>11</SUP> cm<SUP>-3</SUP> andtemperatures
  8000-15000 K. Outlying loop systems might be formed by magnetic
  fieldreconnection, analogous to the mechanism ascribed to eruptive
  two-ribbon flares, butassociated with field structures adjacent to the
  flare. Alternatively, these outlying loopsystems may not erupt but
  become visible as a result of heating and chromospheric evaporation
  at the footpoints shared with the flare ribbon. In either case, the
  observations presented here have interesting implications for both
  the spatial scale and the topology of thecoronal magnetic fields in
  which eruptions occur.

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Title: The first results from SOHO.
Authors: Fleck, B.; Švestka, Z.
1997frfs.book.....F    Altcode:
  This volume contains papers reporting the first scientific results from
  the SOHO mission as well as descriptions of the in-flight performance of
  some of the instruments. A CD-ROM with multimedia material is included
  as an integral part of this volume. Reprinted from Sol. Phys., Vol. 170,
  No. 1 (Jan 1997) (see AAA, Vol. 67) and Vol. 175, No. 2 (Oct 1997)
  (see AAA, Vol. 68).

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Title: Speeds of Rising Post-Flare Structures
Authors: Švestka, Zdeněk
1996SoPh..169..403S    Altcode:
  There are basically two kinds of post-flare coronal structures: those
  rising with decreasing speed, and others which rise with constant speed
  for a long period of time. As a rule, those structures with decreasing
  speed are post-flare loop systems, while those rising with constant
  speed are postflare giant arches. However, there are exceptions. We
  demonstrate several cases of post-flare loop systems which rise with
  constant speed for many hours, three of them observed by Yohkoh. These
  observations imply that the Kopp and Pneuman interpretation of
  post-flare loops as sequentially reconnecting open field lines
  cannot be generally valid. The most likely interpretation is that all
  post-flare loop systems start with the Kopp and Pneuman process, but
  in some of them later-formed loops begin to be continuously heated;
  thus they cease to cool and begin to expand into the corona. This kind
  of post-flare loops might represent an intermediate stage between the
  ordinary post-flare loops and post-flare giant arches.

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Title: Book reviews
Authors: Howard, R. F.; van den Oord, G. H. J.; Švestka, Z.
1996SoPh..169..225H    Altcode:
  No abstract at ADS

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Title: Large-scale active coronal phenomena in Yohkoh SXT images
Authors: Fárník, František; Švestka, Zdeněk; Hudson, Hugh S.;
   Uchida, Yutaka
1996SoPh..168..331F    Altcode: 1996SoPh..168..331U
  We discuss Yohkoh SXT observations of stationary giant post-flare
  arches which occurred on 3-6 May, 1992 and study in detail the last
  arch, associated with the flare at 19:02 UT on 5 May, which extended
  above the west limb. The arch was similar to the first giant arch
  discovered on board the SMM, on 21-22 May, 1980. We demonstrate that
  the long lifetimes of these structures necessarily imply additional
  energy input from the underlying active region: otherwise, conduction
  would cool these arches in less than one hour and even with the
  unlikely assumption of conduction inhibited, pure radiative cooling
  would not produce the temperature decrease observed. All arch tops,
  although varying in brightness, stayed for several days at a fairly
  constant altitude of ∼ 100 000 km, and the arch studied, on 5-6 May,
  was just a new brightening of the pre-existing decaying structure. The
  brightening was apparently due to inflow of hot plasma from the flare
  region. Yohkoh data confirm that these stationary arches are rare
  phenomena when compared with the rising arches studied in Paper I and
  with Uchida et al.'s expanding active regions.

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Title: Flare-like dynamic phenomena
Authors: Rompolt, B.; Švestka, Z.
1996AdSpR..17d.115R    Altcode: 1996AdSpR..17..115R
  Using data from Skylab, SMM, and Yohkoh spacecraft, as well as Hα
  observations on the ground, we summarize the present knowledge about
  dynamic phenomena on the Sun which usually are not classified as
  flares, although they resemble processes observed in flares, often are
  associated with flares, and sometimes can be considered for special
  kinds of flares. This involves field openings outside active regions
  (eruptive flares without chromospheric response), loop eruptions,
  with emphasis on brightenings (and possibly eruptions) of loops which
  interconnect active regions, sprays, flaring arches (injections of
  hot and cool plasma into closed field configurations), Hα and X-ray
  surges (injections of hot and cool plasma into `open' fields), X-ray
  jets, recently discovered by Yohkoh, as well as Hα jets observed at
  Wroclaw and Ottawa. We will try to find relationships between all the
  latter phenomena so that one gets a more homogeneous picture of plasma
  injections and jets observed on the Sun. There are many active phenomena
  on the Sun which usually are not classified as flares, although they
  closely resemble processes observed in flares, or are very often,
  and quite typically, associated with flares. Some of them are even
  caused by the same kind of instability that produces flares.

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Title: Large-Scale Active Coronal Phenomena in YOHKOH SXT Images
Authors: Svestka, Z.; Farnik, F.; Hudson, H. S.; Uchida, Y.; Hick, P.
1996ASPC..111..388S    Altcode: 1997ASPC..111..388S
  The authors have checked in Yohkoh SXT images the appearance of giant
  post-flare arches which were discovered in hard X-ray images from
  the HXIS and FCS instruments onboard the SMM. They have verified the
  existence of both the rising and stationary arches. In addition to
  these two kinds of giant post-flare arches, known before from SMM
  observations, Yohkoh also reveals other large post-flare coronal
  structures which might have been considered to be giant arches by the
  low-resolution SMM instruments. These include coronal helmet streamers
  above rising flare loops or fans of hot structures in which the rising
  loops are embedded.

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Title: Large-Scale Active Coronal Phenomena in YOHKOH SXT Images
Authors: Svestka, Z.; Farnik, F.; Hudson, H. S.; Uchida, Y.; Hick,
   P.; Lemen, J. R.
1996mpsa.conf..609S    Altcode: 1996IAUCo.153..609S
  No abstract at ADS

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Title: Coronal phenomena associated with flares.
Authors: Svestka, Z.
1996joso.proc..135S    Altcode:
  The paper reviews various kinds of large-scale coronal phenomena which
  are associated with solar flares. Particular attention is paid to Hα
  and X-ray observations of "post"-flare loops and to recent Yohkoh
  observations of slowly expanding giant arches and extensive "ray"
  structures embedding flare loop systems.

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Title: Large-Scale Active Coronal Phenomena in YOHKOH SXT Images, I
Authors: Švestka, Zdeněk; Fárník, František; Hudson, Hugh S.;
   Uchida, Yutaka; Hick, Paul; Lemen, James R.
1995SoPh..161..331S    Altcode:
  We have found several occurrences of slowly rising giant arches inYohkoh
  images. These are similar to the giant post-flare arches previously
  discovered by SMM instruments in the 80s. However, we see them now
  with 3-5 times better spatial resolution and can recognize well their
  loop-like structure. As a rule, these arches followeruptive flares
  with gradual soft X-ray bursts, and rise with speeds of 1.1-2.4 km
  s<SUP>−1</SUP> which keep constant for &gt;5 to 24 hours, reaching
  altitudes up to 250 000 km above the solar limb. These arches differ
  from post-flare loop systems by their (much higher) altitudes, (much
  longer) lifetimes, and (constant) speed of growth. One event appears
  to be a rise of a transequatorial interconnecting loop.

---------------------------------------------------------
Title: On `The Solar Flare Myth' postulated by Gosling
Authors: Švestka, Zdeněk
1995SoPh..160...53S    Altcode:
  The `Solar Flare Myth' postulated by Gosling (1993) is
  a misunderstanding. It is true that most sources of coronal mass
  ejections (CMEs) cannot be classified as flares in the common old sense
  of that word. However, just for this reason the term `eruptive flare'
  has been introduced for all solar active phenomena in which an opening
  of field lines is involved and which lead to magnetic-field and mass
  ejections resulting in a CME. The process is essentially the same in all
  events, irrespective of' whether only adisparition brusque without any
  chromospheric brightening or a major two-ribbon flare is involved in it;
  the only difference is the different strength of the magnetic field in
  which the process was accomplished. The major two-ribbon (cosmic-ray)
  flares clearly represent the most energetic events of this kind, and,
  therefore, it is very misleading to claim that solar flares in general
  are phenomena with very little importance for solar-terrestrial physics.

---------------------------------------------------------
Title: A comparison of solar activity during the decline of several
    solar cycles
Authors: Svestka, Z.
1995AdSpR..16i..27S    Altcode: 1995AdSpR..16R..27S
  This review summarizes the general characteristics of solar activity
  during the declining part of solar cycles and compares the behavior
  of the Sun during several last cycles. Different characteristics of
  solar activity are considered and tentative reasons for their different
  behavior in different cycles are suggested. The activity decline is
  usually very irregular, characterized by quiet periods interrupted by
  temporary bursts of activity. These bursts can be quite impressive:
  actually, as a rule, the most outstanding events of solar activity do
  not occur at the cycle maximum, but shortly before it, or a few years
  later. The duration of quiet periods between activity enhancements
  increases as the cycle declines, but even close to the solar minimum
  one may still encounter quite interesting flare events. From the
  point of view of solar-terrestrial relations, these late events are
  particularly favorable, because their effects in interplanetary space
  and in planetary magnetospheres can be followed much easier than
  during high solar activity: one can uniquely ascribe the observed
  consequencies in space to their isolated sources on the Sun.

---------------------------------------------------------
Title: Book Review: Planetary systems : formation, evolution and
    detection / Kluwer, 1994
Authors: Solanki, S. K.; Švestka, Zdeněk; Svestka, Z.
1995SoPh..159..403S    Altcode: 1995SoPh..159..403B
  No abstract at ADS

---------------------------------------------------------
Title: Flare-Associated Darkenings in H-Alpha: Possible Evidence
    for Faint Outlying, Unresolved Loop Systems
Authors: Neidig, D. F.; Cliver, E. W.; Svestka, Z.; Airapetian, V.;
   Henry, T. W.
1995SPD....26.1215N    Altcode: 1995BAAS...27..986N
  No abstract at ADS

---------------------------------------------------------
Title: The Participation of Nuclei in Type-Iii Related Electron
    Streams
Authors: Kallenrode, May-Britt; Svestka, Zdenek
1994SoPh..155..121K    Altcode:
  We study 27 increases of the flux of 300-800 keV electrons on board
  HELIOS A or B, associated with intense type III radio bursts close
  to perihelion passages of the two spacecraft, during the solar
  minimum. Electrons can be detected inside cones with an angular
  width between 30° and 60°. Though only intense type III bursts
  are associated with recognizable electron events in space, such
  an association does not exist for all of them; this fact and great
  differences in fluxes of the individual events indicate that, apart
  from the intensity, also some other charactefistic of the type III
  burst acceleration or propagation process determines the resulting
  flux of electrons in space; the energy spectrum of the accelerated
  electrons is one of the likely candidates. A comparison of the electron
  flux in these events with the flux of 1.7-3.7 MeV nucl<SUP>−1</SUP>
  helium reveals very large variations of the helium/electron flux ratio,
  by a factor of at least 15 and possibly much higher. We demonstrate that
  these variations are not caused by propagation effects in interplanetary
  space. Therefore, they must be due either to propagation effects in the
  solar corona or, more likely, to intrinsic variations in the relative
  production of electrons and nuclei in the type III burst process. An
  extrapolation of the observed fluxes to 1 AU shows that in only 7 of
  the 27 electron events studied might a marginal &gt; 1.7 MeV helium
  flux be recognized ar the Earth distance.

---------------------------------------------------------
Title: On the Occurrence of Blue Asymmetry in Chromospheric Flare
    Spectra
Authors: Heinzel, Petr; Karlicky, Marian; Kotrc, Pavel; Svestka, Zdenek
1994SoPh..152..393H    Altcode:
  We present observations of optical spectra of a flare in which blue line
  asymmetry was seen for more than 4 min close to the flare onset. The
  maximum blue asymmetry coincided with the maximum of a hard X-ray
  and microwave burst. We discuss possible interpretations of the blue
  asymmetry and conclude that the most plausible one is electron-beam
  heating with return current. Although this process predicts downflows
  in the lower transition region and upper chromosphere, its ultimate
  effect on the line profiles can be blue asymmetry: the upper layers
  moving away from us absorb the radiation of the red peak thus lowering
  its intensity in comparison to the blue one.

---------------------------------------------------------
Title: Slow-mode oscillations of large-scale coronal loops
Authors: Svestka, Zdenek
1994SoPh..152..505S    Altcode:
  On several occasions, repetitive X-ray brightenings, sometimes
  accompanied by mass injections into adjacent loops, appeared
  quasi-periodically with mean periods close to 20 minutes. In all cases
  when X-ray images were available, the sites of these brightenings were
  in active regions which were associated with large-scale coronat loops
  of length (2 − 3) × 10<SUP>5</SUP> km. Therefore, the primary source
  of these long-periodic pulsations might be slow-mode oscillations in
  these large-scale loops. Free MHD oscillations, proposed earlier by
  Roberts, Edwin, and Benz (1984), may fit the observed data.

---------------------------------------------------------
Title: Book-Review - Space Science Dictionary
Authors: Kleczek, J.; Ckeczkova, H.; Svestka, Z.
1994SoPh..151..203K    Altcode:
  No abstract at ADS

---------------------------------------------------------
Title: Book review
Authors: Švestka, Z.
1994SoPh..151..203S    Altcode:
  No abstract at ADS

---------------------------------------------------------
Title: X-Ray Observations of a Major Eruptive Flare Behind the Limb
Authors: Smith, Kermit L.; Strong, Keith T.; Švestka, Zdeněk;
   McCabe, Marie K.
1994SoPh..149..363S    Altcode:
  We analyze X-ray images and spectra of a coronal structure which
  extended to altitudes over 130 000 km above an eruptive flare located
  20° behind the western solar limb. The images were obtained by the
  Flat Crystal Spectrometer (FCS) and the spectra were obtained by the
  Bent Crystal Spectrometer (BCS) aboard the SMM spacecraft. Images
  in OVIII and MgXI lines cover the period from before the flare onset
  (which occurred at 22:31 UT on 16 February, 1986) through 17 UT on 17
  February and were used for determination of temperature and emission
  measure within the structure. BCS obtained CaXIX spectra of the coronal
  event, benefiting from the occultation of the active region behind
  the solar limb.

---------------------------------------------------------
Title: Large-Scale Coronal Structures Associated with Solar Activity
    (Invited)
Authors: Svestka, Z.; Farnik, F.
1994scs..conf..243S    Altcode: 1994IAUCo.144..243S
  The authors summarize observations of filament eruptions, post-flare
  loops, giant post-flare arches, flaring arches, surges, coronal
  responses to chromospheric brightenings, and interconnecting loops,
  made by Skylab and SMM, and confront some of them with soft X-ray
  observations recently made by Yohkoh. It seems likely that many
  structures observed by Yohkoh are the same phenomena that were seen
  before, but it may be sometimes difficult to identify them correctly.

---------------------------------------------------------
Title: Book-Review - Astronomy and Astrophysics Abstracts - Index
    - V.51-55
Authors: Burkhardt, B.; Esser, U.; Hefele, H.; Heinrich, I.; Hofmann,
   W.; Krahn, D.; Matas, V. R.; Schmadel, L. D.; Wielen, R.; Zech, G.;
   Svestka, Z.
1993SoPh..148..177B    Altcode:
  No abstract at ADS

---------------------------------------------------------
Title: Book review
Authors: Švestka, Z.
1993SoPh..148..177S    Altcode:
  No abstract at ADS

---------------------------------------------------------
Title: Book-Review - the YOHKOH Solar-A Mission
Authors: Svestka, Z.; Uchida, Y.; Farnik, F.
1993SSRv...64..367S    Altcode:
  No abstract at ADS

---------------------------------------------------------
Title: An Analysis of SKYLAB X-Ray Pictures of a Giant Coronal Arch
Authors: Simberova, Stanislava; Karlicky, Marian; Svestka, Zdenek
1993SoPh..146..343S    Altcode:
  The limb event of 13/14 August, 1973, imaged by Skylab in soft X-rays,
  proved to be a giant arch, quite similar to those observed in 1980-1986
  on SMM. High spatial resolution (by a factor of 4-5 better than in SMM
  data) made it possible to see the internal structure of the arch. Its
  brightest part consisted of loops very similar to, but higher than,
  post-flare loops, surrounded by a rich system of weak loop structures
  extending up to altitudes of 260 000 km. While the main brightest
  structure of the arch was newly formed, the weak very large loops had
  existed above the active region before and were only enhanced during
  the event.

---------------------------------------------------------
Title: Responses of large-scale coronal structures to chromospheric
    activity
Authors: Farnik, Frantisek; Hick, Paul; Svestka, Zdenek
1993SoPh..146..313F    Altcode:
  We have followed the transit of two active regions across the western
  solar limb during June 29 through July 2, 1980, as imaged in 3.5-16
  keV X-rays by HXIS aboard the SMM. During frequent brightenings of
  large-scale coronal structures, hard X-ray emission in the 11-16 keV
  energy band was recorded up to altitudes of 76 000 km. Soft X-rays
  could be seen in excess of 250 000 km altitude above the photospheric
  active region. Many X-ray brightenings low in the corona in the
  active regions were followed by enhancements high in the corona in
  the large-scale coronal structures. Although subsequent enhancements
  rarely appeared in the same position, similar portions of the corona
  brightened intermittently, indicating that the general configuration
  of the coronal structures above the active regions did not change much,
  in spite of the frequent energy inputs. These inputs were of two kinds:
  nonthermal, with very fast response at high coronal altitudes within
  seconds or tens of seconds, and thermal, with a delay of several
  minutes. The nonthermal response is short-lived, reflecting the time
  profile of the primary source; the thermal response is more gradual
  and longer lasting than the primary source. In some enhancements of
  large-scale coronal structures both these kinds of response occur and
  can be clearly recognized. There are also active-region hrightenings
  without any response in the high corona and,vice versa, high-corona
  brightenings without any obvious primary source; in the latter case,
  it is likely that the source was hidden behind the limb.

---------------------------------------------------------
Title: Book-Review - the YOHKOH Solar-A Mission
Authors: Svestka, Z.; Uchida, Y.; Bromage, B.
1993Obs...113..165S    Altcode:
  No abstract at ADS

---------------------------------------------------------
Title: Editorial
Authors: de Jager, Cornelis; Howard, Robert F.; švestka, Zdeněk
1993SoPh..143D...7D    Altcode:
  No abstract at ADS

---------------------------------------------------------
Title: Book-Review - Eruptive Solar Flares
Authors: Svestka, Z.; Jackson, B. V.; Machado, M. E.; Sylwester, J.
1993SSRv...65..186S    Altcode:
  No abstract at ADS

---------------------------------------------------------
Title: X-Ray Observations of Limb Flare Loops and Post-Flare
    Coronal Arch
Authors: Svestka, Zdenek; Smith, Kermit L.; Strong, Keith T.
1992SoPh..139..405S    Altcode:
  We present observations of another post-flare arch following an
  eruptive flare, detected in X-ray lines above the western solar limb
  on 2 May 1985.

---------------------------------------------------------
Title: Book-Review - the YOHKOH / Solar-A Mission
Authors: Svestka, Z.; Uchida, Y.
1992JBAA..102R.109S    Altcode:
  No abstract at ADS

---------------------------------------------------------
Title: Book-Review - the YOHKOH Solar-A Mission
Authors: Svestka, Z.; Uchida, Y.
1992JBAA..102Q.109S    Altcode:
  No abstract at ADS

---------------------------------------------------------
Title: Book-Review - the YOHKOH Solar-A Mission
Authors: Svestka, Z.; Uchida, Y.
1992Sci...256R.253S    Altcode:
  No abstract at ADS

---------------------------------------------------------
Title: The Birth of Giant Post-Flare Arches
Authors: Poletto, G.; Svestka, Z.
1992SoPh..138..189P    Altcode:
  Using short accumulation times, we have succeeded in the detection
  in HXIS images of the initial growth of the giant post-flare arch
  of 6 November, 1980 at 14:44 UT and part of the initial growth of
  the giant arch of 7 November, 1980 at 04:30 UT. These observations
  are relevant to the problem of the origin of giant arches: the fact
  that the arch of 6 November was imaged more than half an hour before
  the first flare loops had been recorded in the associated flare,
  proves that giant arches cannot: be interpreted as upper products of
  the reconnection process that creates the growing systems of flare
  loops (as the original interpretation by Švestka et al. (1982a)
  suggested). However, also the alternative hypothesis by Poletto and Kopp
  (1988) that these structures originate through a reconnection process
  in a peripheral, large-scale configuration meets with difficulties:
  after the initial rise, the maximum brightness in both arches seems
  to descend, until a much slower rise was resumed about two hours later.

---------------------------------------------------------
Title: Editorial
Authors: de Jager, Cornelis; Švestka, Zdeněk; Howard, Robert F.
1992SoPh..137D...5D    Altcode:
  No abstract at ADS

---------------------------------------------------------
Title: History and Basic Characteristics of Eruptive Flares
Authors: Svestka, Z.; Cliver, E. W.
1992LNP...399....1S    Altcode: 1992esf..coll....1S; 1992IAUCo.133....1S
  We review the evolution of our knowledge and understanding of the
  eruptive (dynamic, two-ribbon) flare phenomenon. Starting with the
  first observation of a white-light flare by Carrington and Hodgson in
  1859, we cover in succession the highlights: Hale's invention of the
  spectroheliograph in 1892 and the spectrohelioscope in 1926 started
  flare observations in H. The institution of a world-wide flare patrol
  brought significant advances in knowledge of flares in the 1930s and
  1940s and new windows were opened to observe flares at short (SID) and
  long (radio) wavelengths. In the 1950s and 1960s metric radio bursts
  were related to trapped energetic electrons and shocks, and two-ribbon
  flares were associated with energetic protons in space. Radio and X-ray
  observations gave evidence for two basic types of flare processes:
  an impulsive phase followed by a long-duration or gradual phase. It
  was found that flares were often preceded by filament activations, and
  growing loop prominence systems were recognized as the limb counterpart
  of two-ribbon disk flares. The early 1970s brought Skylab observations
  of coronal mass ejections (CMEs) and arcades of coronal soft X-ray
  loops above two-ribbon flares. In the mid-1970s, the Kopp-Pneuman
  reconnection model, based on configurations proposed earlier by
  Carmichael, Sturrock, and Hirayama, provided a framework in which the
  newly discovered CMEs could be related to the basic characteristics
  of two-ribbon flares. The 1980s brought, key new results from SMM
  and Hinotori including images of hard X-ray flares and large-scale
  coronal structures associated with eruptive flares. In the conclusion,
  we summarize the basic characteristics of eruptive flares.

---------------------------------------------------------
Title: Eruptive Solar Flares
Authors: Svestka, Zdenek; Jackson, Bernard V.; Machado, Marcos E.
1992LNP...399.....S    Altcode: 1992IAUCo.133.....S; 1992esf..coll.....S
  This is an exhaustive survey of present-day solar research including
  both theory and observations. It deals with eruptive flares, filament
  eruption in x-rays and radio waves, energy release and transport, and
  terrestrial response to solar flares. Details of the most recent SOLAR-A
  project (launched shortly after the conference) are also presented.

---------------------------------------------------------
Title: A Giant Post-Flare Coronal Arch Observed by SKYLAB
Authors: Svestka, Z.; Simberova, S.
1992LNP...399..221S    Altcode: 1992esf..coll..221S; 1992IAUCo.133..221S
  The limb event of 13 August 1973, observed by Skylab in soft X-rays,
  exhibited typical characteristics of the giant post-flare arches
  observed by HXIS and FCS on board SMM in the 1980s. We present here
  examples of the processed Skylab images which yield 4 times better
  angular resolution than the SMM experiments and thus, for the first
  time, make it possible to distinguish the real fine structure of a
  giant post-flare arch.

---------------------------------------------------------
Title: A Giant Coronal Arch Observed by Skylab
Authors: Švestka, Zdeněk
1991SoPh..135..419S    Altcode:
  The limb event of 13 August 1973, observed by Skylab in soft X-rays, has
  all the typical characteristics of the giant post-flare arches observed
  by HXIS and FCS on board SMM in the 1980s. Skylab images provide us
  with 4-5 times better angular resolution than the SMM experiments and
  thus, for the first time, make it possible to distinguish the real
  fine structure of a giant post-flare arch. The image processing of
  the 13/14 August 1973 event is now in progress.

---------------------------------------------------------
Title: Book-Review - Astronomy and Astrophysics Abstracts V.49A/B
Authors: Burghardt, G.; Esser, U.; Hefele, H.; Heinrich, I.; Hofmann,
   W.; Krahn, D.; Matas, V. R.; Schmadel, L. D.; Wielen, R.; Zech, G.;
   Svestka, Z.
1991SoPh..134..411B    Altcode:
  No abstract at ADS

---------------------------------------------------------
Title: Book reviews
Authors: Švestka, Z.
1991SoPh..134..411S    Altcode:
  No abstract at ADS

---------------------------------------------------------
Title: Flaring Arches - Part Three
Authors: Fontenla, Juan M.; Svestka, Zdenek; Farnik, Frantisek; Tang,
   Frances Y.
1991SoPh..134..145F    Altcode:
  We show detailed observations in X-rays, UV lines, and Hα of an
  extended arch, about 300000 km long, which developed as a consequence
  of a compact subflare. This subflare occurred in an `included' magnetic
  polarity of relatively low magnetic field strength (compared to that of
  the sunspots). The apparition of this big arch was preceded by that of a
  smaller arch, about 30000 km long, which masked the polarity inversion
  line filament in the early phase of the subflare. The big arch which
  developed later, around the time of the main X-ray and UV spike of the
  subflare, connected the included polarity and the main leading sunspot
  of the region, and became fully developed in a few minutes. The fact
  that both arches were simultaneously observed in all spectral domains as
  well as their fine structure in Hα can only be explained by considering
  the arch as composed of several unresolved portions of material
  having widely different temperatures. The Hα observations can be
  interpreted as showing the appearance of this cool material as a result
  of condensation, but a more appealing interpretation is that there
  was almost simultaneous ejection of superhot (10<SUP>7</SUP> K), hot
  (10<SUP>6</SUP> K), mild (10<SUP>5</SUP> K), and cool (10<SUP>4</SUP>
  K) material from the subflare site along previously existing magnetic
  tubes of much lower density. The termination of the subflare was marked
  by a rather hard X-ray and UV spike which appeared to originate in a
  different structure than that of the main spike. The material in the
  arch gradually cooled and drained down after the end of the subflare.

---------------------------------------------------------
Title: Book reviews
Authors: Hudson, H. S.; Kleczek, J.; Švestka, Z.
1991SoPh..133..403H    Altcode:
  No abstract at ADS

---------------------------------------------------------
Title: The YOHKOH (Solar-A) Mission : a series of invited
    contributions
Authors: Svestka, Zdenek; Uchida, Yutaka
1991ysam.book.....S    Altcode: 1991QB526.F6Y64....
  No abstract at ADS

---------------------------------------------------------
Title: Needs and constraints for solar flares space-borne cooperative
    programs.
Authors: Svestka, Z.
1991AdSpR..11e.115S    Altcode: 1991AdSpR..11Q.115S
  There are three basic reasons for cooperation in space observations of
  flares: (1) observations in different spectral regions, (2) stereoscopic
  observations, and (3) in situ data. Using experience from the past
  and considering the planned experiments, problems encountered by
  flare-related cooperative programs on spacecraft are briefly summarized.

---------------------------------------------------------
Title: The YOHKOH (SOLAR-A) mission. A series of invited
    contributions.
Authors: Švestka, Z.; Uchida, Y.
1991yohk.book.....S    Altcode:
  The SOLAR-A spacecraft was launched by the Institute of Space and
  Astronautical Science, Japan (ISAS) in August 1991, and, following
  an ISAS tradition, was renamed YOHKOH. This mission is dedicated
  principally to the study of solar flares, especially of high-energy
  phenomena observed in the X- and gamma-ray ranges. With a coordinated
  set of instruments including hard X-ray and soft X-ray imaging
  telescopes as well as spectrometers with advanced capabilities, it will
  reveal many new aspects of flares and help better understand their
  physics, supporting international collaborations with ground-based
  observatories as well as theoretical investigations. An overview of
  this mission, including the satellite, its scientific instruments,
  and its operation, is given.

---------------------------------------------------------
Title: Evolution of Hot Plasma in Flares
Authors: Svestka, Zdenek F.
1991LNP...387..165S    Altcode: 1991fpsa.conf..165S
  This review discusses, in particular, X-ray manifestations of the
  development of hot flare plasma during the cooling phase of flares. In a
  preexisting coronal configuration, a small flare source can excite much
  larger coronal loops and arches, of which only the footpoints become
  visible if their density is low, or their whole structures can be seen
  if density is high enough. Flaring arches, through which both cool and,
  hot plasma flows from the primary flare source to a secondary footpoint,
  are the most spectacular phenomena of this kind. In other cases the
  flaring loops did not exist before, but have been newly formed during
  the flare process. These are the eruptive flares, in which the preflare
  field lines are first disrupted and subsequently reconnect. The main
  part of this review is devoted to the development of hot plasma in
  this particular kind of flaring structures. It is emphasized that
  X-ray observations of growing systems of loops in eruptive flares,
  and giant arches following these flares high in the corona, require
  large fields of view pointed for several hours at the active region in
  which the flare occurred. This makes their observations with SOLAR-A
  rather difficult, but one should realize that SOLAR-A represents the
  only means for studying these coronal components of the most important
  solar flares until, at least, the end of this century.

---------------------------------------------------------
Title: Real-time simulation of a potential magnetic field in a
    post-flare arch
Authors: Poletto, Giannina; Svestka, Zdenek
1990SoPh..129..363P    Altcode:
  We analyze the X-ray observations on 7-8 November of the last revival
  of a giant coronal arch first observed in the morning hours of 6
  November, 1980. We compare these data with observations of earlier
  revivals of this arch, in order to determine whether the successive
  brightenings repeat without any apparent modification, or whether they
  show a varying behavior as they keep occurring. We also examine the
  magnetic structure of the revived arches in order to ascertain whether
  the subsequent phenomena involve the same magnetic configuration. The
  information about the magnetic structure of the last revival is the
  best we have, because the revival started close to the time of the
  Kitt Peak magnetogram which has been used for the magnetic modelling
  of the whole series of these giant arches.

---------------------------------------------------------
Title: X-Ray Bright Surges
Authors: Svestka, Zdenek; Farnik, Frantisek; Tang, Frances
1990SoPh..127..149S    Altcode:
  We present evidence of X-ray emission from surges that are bright
  in Hα. These surges have many features common to flaring arches of
  Martin and Švestka (1988); the basic difference between the two is
  that in flaring arches cold and hot plasma are injected into clearly
  defined closed magnetic loops, while in the surges the injection
  goes into large-scale magnetic field structures of which the second
  footpoint is usually unknown. Because of the steep density gradient in
  such large-scale structures, the X-ray visibility of bright surges is
  limited to a few tens of seconds only. A series of repetitive surges,
  some of them bright and emitting X-rays, occurred on 8 July, 1980
  from footpoints of two large-scale coronal structures, which might
  have been the legs of an enormous arch at least 600 Mm long.

---------------------------------------------------------
Title: Book-Review - Astronomy and Astrophysics Abstracts
Authors: Esser, U.; Hefele, H.; Heinrich, I.; Hofmann, W.; Krahn,
   D.; Matas, V. R.; Schmadel, L. D.; Zech, G.; Svestka, Z.
1990SoPh..126..411E    Altcode:
  No abstract at ADS

---------------------------------------------------------
Title: Book Review: The sun: an introduction / Springer-Verlag
Authors: Mewe, R.; Švestka, Z.; Mewe, R.
1990SoPh..126..411M    Altcode: 1990SoPh..126..411S
  No abstract at ADS

---------------------------------------------------------
Title: Book-Review - Astronomy and Astrophysics Abstracts V.44
Authors: Bohme, S.; Svestka, Z.
1989SoPh..119..420B    Altcode:
  No abstract at ADS

---------------------------------------------------------
Title: Book Review: Solar and stellar physics. / Springer-Verlag, 1987
Authors: Poletto, Giannina; Dimitrov, D. L.; Švestka, Z.; Poletto, G.
1989SoPh..119..419P    Altcode: 1989SoPh..119..419S
  No abstract at ADS

---------------------------------------------------------
Title: Flaring Arches - Part Two
Authors: Svestka, Zdenek; Farnik, Frantisek; Fontenla, Juan M.;
   Martin, Sara F.
1989SoPh..123..317S    Altcode:
  We discuss first the development of the coronal arch-shaped structure of
  ∼ 57000 km length which was born at or before 08:00 UT on 6 November,
  1980 and became the site of 13 quasi-periodic brightenings in hard
  X-rays from 10:00 to 14:30 UT. The same structure became the site
  of a series of 17 flaring arches between 15:30 and 24:00 UT on that
  day. The periodicity of ∼ 19 min, defined well for the quasi-periodic
  variations, seems to be partly retained during the occurrence of the
  flaring arches.

---------------------------------------------------------
Title: The Footpoints of Giant Arches
Authors: Martin, Sara F.; Svestka, Zdenek F.; Bhatnagar, Arvind
1989SoPh..124..339M    Altcode:
  We have detected chromospheric footpoints of the giant post-flare
  coronal arches discovered by HXIS a few years ago. Hα photographs
  obtained at Big Bear and Udaipur Solar Observatories show chromospheric
  signatures associated with 5 sequential giant arch events observed
  in the interval from 6 to 10 November, 1980. The set of footpoints at
  one end of the arches consists of enhancements within a plage at the
  northeast periphery of the active region and the set of footpoints at
  the other end of the arch consists of brightenings of the chromosphere
  south of the active region. Both sets of footpoints show very slow
  brightness variations correlated in time with the brightness variations
  of the X-ray arches. Current-free modelling of the coronal magnetic
  field by Kopp and Poletto (1989), based on a Kitt Peak magnetogram,
  confirms the identification of the two sets of footpoints by showing
  magnetic field lines connecting them.

---------------------------------------------------------
Title: Solar Flares - the Gradual Phase
Authors: Svestka, Zdenek
1989SoPh..121..399S    Altcode: 1989IAUCo.104..399S
  One has to distinguish between two kinds of the gradual phase of flares:
  (1) a gradual phase during which no energy is released so that we see
  only cooling after the impulsive phase (a confined flare), and (2)
  a gradual phase during which energy release continues (a dynamic flare).

---------------------------------------------------------
Title: Book-Review - Astronomy and Astrophysics Abstracts
Authors: Esser, U.; Hefele, H.; Heinrich, I.; Hofmann, W.; Krahn,
   D.; Matas, V. R.; Schmadel, L. D.; Zech, G.; Svestka, Z.
1989SoPh..124..193E    Altcode:
  No abstract at ADS

---------------------------------------------------------
Title: Book-Review - Reports on Astronomy Transactions of the
    International Astronomical Union
Authors: Švestka, Zdeněk
1989SoPh..122..191S    Altcode:
  No abstract at ADS

---------------------------------------------------------
Title: Editorial
Authors: de Jager, Cornelis; Švestka, Zdeněk; Howard, Robert F.
1989SoPh..121D...9D    Altcode:
  No abstract at ADS

---------------------------------------------------------
Title: Giant solar arches and coronal mass ejections in November 1980
Authors: Svestka, Zdenek F.; Jackson, Bernard V.; Howard, Russell A.;
   Sheeley, Neil R., Jr.
1989SoPh..122..131S    Altcode:
  Using data from the SOLWIND coronagraph and photometers aboard
  HELIOS-A we examine coronal mass ejections from an active region
  which produced a series of giant post-flare coronal arches. HXIS
  X-ray observations reveal that in several cases underlying flares
  did not disrupt these arch structures, but simply revived them,
  enhancing their temperature, density and brightness. Thus we are
  curious to know how these quasi-stationary X-ray structures could
  survive in the corona in spite of recurrent appearances of powerful
  dynamic flares below them. We have found reliable evidence that two
  dynamic flares which clearly revived the preexisting giant arch were
  not associated with any mass ejection. After two other flares, which
  were associated with mass ejections, the arch might have been newly
  formed when the ejection was over. In one of these cases, however,
  the arch had typical characteristics of a revived structure so that
  it is likely that it survived a powerful mass ejection nearby. In a
  magnetic configuration of the arch which results from potential-field
  modelling (Figure 1(b)) such a survival seems possible.

---------------------------------------------------------
Title: Book Review: The physics of solar flares. / CUP, 1988
Authors: Svestka, Z.
1989SoPh..122..192S    Altcode: 1989SoPh..122..192T
  No abstract at ADS

---------------------------------------------------------
Title: Coronal mass ejections and coronal structures.
Authors: Hildner, E.; Bassi, J.; Bougeret, J. L.; Duncan, R. A.;
   Gary, D. E.; Gergely, T. E.; Harrison, R. A.; Howard, R. A.; Illing,
   R. M. E.; Jackson, B. V.; Kahler, S. W.; Kopp, K.; Low, B. C.; Lantos,
   P.; Phillips, K. J. H.; Poletto, G.; Sheeley, N. R., Jr.; Stewart,
   R. T.; Svestka, Z.; Waggett, P. W.; Wu, S. T.
1989epos.conf..493H    Altcode:
  The work of this team was concerned with modelling of post-flare arches,
  the reconnection theory of flares, the slow variation of coronal
  structure, and the coronal and interplanetary detection, evolution,
  and consequences of mass ejections.

---------------------------------------------------------
Title: Book-Review - Astronomy and Astrophysics Abstracts
Authors: Bohme, S.; Svestka, Z.
1988SoPh..115..409B    Altcode:
  No abstract at ADS

---------------------------------------------------------
Title: Solar and interplanetary observations of the mass ejection
    on 7 May, 1979
Authors: Jackson, Bernard V.; Rompolt, Bogdan; Svestka, Zdenek
1988SoPh..115..327J    Altcode:
  We present observations of a mass ejection that was observed by five
  different instruments along its way from the solar surface to more
  than 100 solar radii. The instruments involved are the ground-based
  Hα coronagraph at Wrocław, the white-light SOLWIND coronagraph on
  board the P78-1 satellite, zodiacal light photometers of the HELIOS
  B spacecraft, in situ plasma detectors and magnetometers on board the
  HELIOS B spacecraft, and interplanetary scintillation measurements on
  the ground. By using a CAT-scan analysis of the images obtained by the
  SOLWIND coronagraph near the Earth and HELIOS B photometers placed at
  0.3 AU perpendicular to the Earth-Sun line, we have been able to get a
  three-dimensional density reconstruction of the mass ejection and fit
  the best velocity curve for its propagation. Although problems exist
  in smoothly joining the height-time curves (for instance, we had to
  reduce the brightness of the SOLWIND data by more than a factor of two
  to make the data sets agree photometrically), both this analysis and
  direct measurements by the other experiments clearly indicate higher
  speeds at greater distances from the Sun. The plasma acceleration
  in this case was obviously not limited only to distances within 3
  R<SUB>0</SUB>, as is usually the case, but continued beyond the outer
  limit of the coronagraph view at ∼ 8 R<SUB>0</SUB>.

---------------------------------------------------------
Title: Book Review: The early universe. / Reidel, 1987
Authors: Kleczek, J.; Švestka, Z.; Kleczek, J.
1988SoPh..115..409K    Altcode: 1988SoPh..115..409U
  No abstract at ADS

---------------------------------------------------------
Title: Book reviews
Authors: Schindler, K.; Švestka, Zdeněk
1988SoPh..114..193S    Altcode:
  No abstract at ADS

---------------------------------------------------------
Title: Book Review: The galaxy and the solar system. / U Arizona
    Press, 1986.
Authors: Kotov, V. A.; Kostik, R.; Shchukina, N.; Švestka, Zdeněk;
   Kotov, V. A.
1988SoPh..115..203K    Altcode: 1988SoPh..115..203S
  No abstract at ADS

---------------------------------------------------------
Title: Flaring Arches - Part One
Authors: Martin, Sara F.; Svestka, Zdenek F.
1988SoPh..116...91M    Altcode:
  `Flaring arches" is a name assigned to a particular component of
  some flares. This component consists of X-ray and Hα emission which
  traverses a coronal arch from one to the other of its chromospheric
  footpoints. The primary footpoint is at the site of a flare. The
  secondary footpoint, tens of thousands of kilometers distant from the
  source flare, but in the same active region, brightens in Hα concurrent
  with the beginning of the hard X-ray burst at the primary site. From the
  inferred travel time of the initial exciting agent we deduce that high
  speed electron streams travelling through the arch must be the source
  of the initial excitation at the secondary footpoint. Subsequently,
  a more slowly moving agent gradually enhances the arch first in
  X-rays and subsequently in Hα, starting at the primary footpoint and
  propagating along the arch trajectory. The plasma flow in Hα shows
  clearly that material is injected into the arch from the site of the
  primary footpoint and later on, at least in some events, a part of it
  is also falling back.

---------------------------------------------------------
Title: Book-Review - Solar Radiophysics
Authors: McLean, D. J.; Labrum, N. R.; Svestka, Z.
1988SoPh..115R.204M    Altcode:
  No abstract at ADS

---------------------------------------------------------
Title: Book-Review - Progress in Solar Physics
Authors: de Jager, C.; Svestka, Z.
1988ApL&C..26..372D    Altcode: 1988ApL....26..372D
  No abstract at ADS

---------------------------------------------------------
Title: Soft X-ray observations of large-scale coronal structures
Authors: Svestka, Zdenek
1988AdSpR...8k..81S    Altcode: 1988AdSpR...8...81S
  This paper draws attention to large-scale structures in the solar corona
  which have been observed only in soft X-rays. Some of them were seen on
  Skylab in 1973 with poor time resolution, some other aboard the SMM with
  poor spatial resolution. The Soft X-ray Telescope on SOLAR-A can see
  them with both kinds of resolution improved by an order of magnitude,
  provided that it images large enough field of view. Three kinds of
  structures are of particular interest: (a) Loops that interconnect
  active regions, even on opposite hemispheres. Observations of their
  birth may provide information both on the basic characteristics of solar
  activity and on solar atmospheric processes (reconnection). Their
  brightenings, losely related to flares, could contribute to our
  knowledge of instabilities in the solar corona. (b) Flaring arches
  inside active regions. They appear in extensive coronal structures
  which may exist for days and intermittently brighten in association
  with intense X-ray bursts. (c) Giant arches which appear for many hours
  high in the corona after dynamic flares. Their structure, mode of birth,
  and their relation to coronal mass ejections, is presently unknown.

---------------------------------------------------------
Title: Thermal Structures Associated with Post-Flare Coronal Arches
Authors: Hick, Paul; Svestka, Zdenek
1987SoPh..108..315H    Altcode:
  Shortly after the dynamic flare of 14 ∶ 44 UT on 6 November, 1980,
  which initiated the second revival in the sequence of post-flare coronal
  arches of 6-7 November, a moving thermal disturbance was observed in
  the fine field of view of HXIS. From 15 ∶ 40 UT until about 18 UT,
  when it left the field of view, the disturbance rose into the corona,
  as indicated by a projected velocity of 7.4 km s<SUP>-1</SUP> in the
  south-east direction. The feature was located above the reconnection
  region of the dynamic flare and was apparently related to the revived
  coronal arch. Observations in the coarse field of view after 18 UT
  revealed a temperature maximum in the revived arch, rising with a
  velocity of 7.0 km s<SUP>-1</SUP> directly in continuation of the
  thermal disturbance. The rise velocity of the disturbance was initially
  (at least until 17 ∶ 20 UT) very similar to the rise velocities
  observed for the post-flare loop tops of the parent flare. This
  suggests that the rise of the reconnection point, in the Kopp and
  Pneuman (1976) mechanism responsible for the rise of the loop tops,
  also dictates the rise of the disturbance. From energy requirements
  it follows that in this phase the disturbed region is still a separate
  magnetic `island', thermally isolated from the old arch structure and
  the post-flare loops. After 18 UT the rise of the post-flare loop tops
  slowed down to 2 km s<SUP>-1</SUP>, which is significantly slower than
  the rise of the brightness and temperature maxima of the revived arch
  in the coarse field of view. Thus in this phase the Kopp and Pneuman
  mechanism is no longer directly responsible for the rise of the thermal
  structure and the rise possibly reflects the merging of the old and
  the new arch structures.

---------------------------------------------------------
Title: Post-flare coronal arches observed with the SMM/XRP Flat
    Crystal Spectrometer
Authors: Hick, Paul; Svestka, Zdenek; Smith, Kermit L.; Strong,
   Keith T.
1987SoPh..114..329H    Altcode:
  The phenomenon of post-flare coronal arches, initially discovered with
  the Hard X-Ray Imaging Spectrometer (HXIS), was investigated using
  observations made with the SMM Flat Crystal Spectrometer (FCS) on 20
  through 23 January, 1985. Since these observations were made with
  a different type of instrument from HXIS, they provide independent
  information on the physical characteristics of the arch phenomenon
  and extend our knowledge to lower coronal temperatures.

---------------------------------------------------------
Title: Highlights of the Flare Build-Up Study
Authors: Gaizauskas, V.; Svestka, Z.
1987SoPh..114..389G    Altcode:
  Years of preparation within the framework of the Flare Build-up
  Study culminated with intensive observations of solar flares during
  the Solar Maximum Year (1979-1981). Scientists operating several
  spacecraft and roughly 70 ground-based observatories participated in
  an internationally coordinated effort to observe flares with higher
  spatial, spectral, and temporal resolution over a wider range of
  wavelengths than heretofore. The FBS stimulated important advances in
  theories of magnetic reconnection and the growth of plasma instabilities
  under preflare circumstances. A series of international FBS workshops
  facilitated data exchanges and collaborative studies for interpreting
  and synthesizing the wealth of new information about flares. The FBS
  ended officially at the Symposium on Synopsis of the Solar Maximum
  Analysis held 2-5 July, 1986 at the COSPAR meeting in Toulouse,
  France. Here we summarize highlights of its progress towards an
  understanding of the storage and release of preflare energy.

---------------------------------------------------------
Title: Multi-thermal observations of newly formed loops in a
    dynamic flare
Authors: Švestka, Zdeněk F.; Fontenla, Juan M.; Machado, Marcos E.;
   Martin, Sara F.; Neidig, Donald F.; Poletto, Giannina
1987SoPh..108..237S    Altcode:
  The dynamic flare of 6 November, 1980 (max ≈ 15:26 UT) developed a
  rich system of growing loops which could be followed in Hα for 1.5
  hr. Throughout the flare, these loops, near the limb, were seen in
  emission against the disk. Theoretical computations of deviations from
  LTE populations for a hydrogen atom reveal that this requires electron
  densities in the loops close to, or in excess of 10<SUP>12</SUP>
  cm <SUP>-3</SUP>. From measured widths of higher Balmer lines the
  density at the tops of the loops was found to be 4 x 10<SUP>12</SUP>
  cm <SUP>-3</SUP> if no non-thermal motions were present, or 5 ×
  10<SUP>11</SUP> cm <SUP>-3</SUP> for a turbulent velocity of ~ 12 km
  s <SUP>-1</SUP>.

---------------------------------------------------------
Title: Cooling of a Coronal Flare Loop Through Radiation and
    Conduction
Authors: Svestka, Zdenek
1987SoPh..108..411S    Altcode:
  A simple method is proposed for a computation of the cooling of coronal
  flare loops by radiation and conduction, for various temperatures,
  densities, and lengths of the loops. The relative importance of
  conductive and radiative losses is briefly discussed.

---------------------------------------------------------
Title: Book-Review - Progress in Solar Physics
Authors: de Jager, C.; Svestka, Z.; Jordan, C.
1987Obs...107..130D    Altcode:
  No abstract at ADS

---------------------------------------------------------
Title: Book-Review - Progress in Solar Physics
Authors: de Jager, C.; Svestka, Z.
1987Sci...236R1009D    Altcode:
  No abstract at ADS

---------------------------------------------------------
Title: Book Review: Of stars and men: reminiscences of an
    astronomer. / Adam Hilger, 1986.
Authors: Svestka, Z.
1987Ap&SS.133..200S    Altcode: 1987Ap&SS.133..200K
  No abstract at ADS

---------------------------------------------------------
Title: Book reviews
Authors: Dyson, John; Švestka, Zdenêk; Kleczek, Josip
1987Ap&SS.133..199D    Altcode:
  No abstract at ADS

---------------------------------------------------------
Title: Book reviews
Authors: Hick, Paul; Jackson, B.; Švestka, Zdenek; Křivský, L.
1987SoPh..108..201H    Altcode:
  No abstract at ADS

---------------------------------------------------------
Title: Book-Review - Astronomy and Astrophysics Abstracts V.42:2
Authors: Bohme, S.; Esser, U.; Hefele, H.; Heinrich, I.; Hofmann,
   W.; Krahn, D.; Matas, V. R.; Schmadel, L. D.; Zech, G.; Svestka, Z.
1987SoPh..114..193B    Altcode:
  No abstract at ADS

---------------------------------------------------------
Title: Relationships among flare images at different wavelengths
Authors: Svestka, Zdenek F.
1987SoPh..113...67S    Altcode: 1982SoPh..113...67S
  The talk reviews briefly historical development of the imaging of the
  Sun, and flare imaging in particular, at different wavelengths. The
  present state is then critically analyzed, emphasizing and demonstrating
  problems related to simultaneity of observed data, differences in time
  resolution, limitations of the imaged field of view, unequal spatial
  resolution, and alignment of the images. Prospects for the future are
  briefly sketched, including imaging in very hard X-rays and γ-rays.

---------------------------------------------------------
Title: Flaring arches
Authors: Martin, Sara F.; Švestka, Zdenek F.
1987SoPh..113..303M    Altcode: 1982SoPh..113..303M
  No abstract at ADS

---------------------------------------------------------
Title: Solar and Interplanetary Observations of the Mass Ejection
    on 7 May 1979
Authors: Jackson, B. V.; Rompolt, B.; Svestka, Z.
1987sowi.conf..272J    Altcode:
  No abstract at ADS

---------------------------------------------------------
Title: Book Review: Transactions of the IAU, Vol. XIXB. / Reidel,
    1986.
Authors: Svestka, Z.
1987SoPh..108..202S    Altcode:
  No abstract at ADS

---------------------------------------------------------
Title: Interplanetary Effects of Coronal Mass Ejections
Authors: Hildner, E.; Bassi, J.; Bougeret, J. L.; Duncan, R. A.;
   Gary, D. E.; Gergely, T. E.; Harrison, R. A.; Howard, R. A.; Illing,
   R. M. E.; Jackson, B. V.; Kahler, S. W.; Kopp, K.; Low, B. C.; Lantos,
   P.; Phillips, K. J. H.; Poletto, G.; Sheeley, N. R., Jr.; Steward,
   R. T.; Svestka, Z.; Waggett, P. W.; Wu, S. T.
1986epos.conf.6.52H    Altcode: 1986epos.confF..52H
  No abstract at ADS

---------------------------------------------------------
Title: Initiations of Coronal Mass Ejections
Authors: Hildner, E.; Bassi, J.; Bougeret, J. L.; Duncan, R. A.;
   Gary, D. E.; Gergely, T. E.; Harrison, R. A.; Howard, R. A.; Illing,
   R. M. E.; Jackson, B. V.; Kahler, S. W.; Kopp, K.; Low, B. C.; Lantos,
   P.; Phillips, K. J. H.; Poletto, G.; Sheeley, N. R., Jr.; Steward,
   R. T.; Svestka, Z.; Waggett, P. W.; Wu, S. T.
1986epos.conf.6.27H    Altcode: 1986epos.confF..27H
  No abstract at ADS

---------------------------------------------------------
Title: The Slowly Varying Corona Near Solar Activity Maximum
Authors: Hildner, E.; Bassi, J.; Bougeret, J. L.; Duncan, R. A.;
   Gary, D. E.; Gergely, T. E.; Harrison, R. A.; Howard, R. A.; Illing,
   R. M. E.; Jackson, B. V.; Kahler, S. W.; Kopp, K.; Low, B. C.; Lantos,
   P.; Phillips, K. J. H.; Poletto, G.; Sheeley, N. R., Jr.; Steward,
   R. T.; Svestka, Z.; Waggett, P. W.; Wu, S. T.
1986epos.conf.6.57H    Altcode: 1986epos.confF..57H
  No abstract at ADS

---------------------------------------------------------
Title: Modelling of Coronal Mass Ejections and POST Flare Arches
Authors: Hildner, E.; Bassi, J.; Bougeret, J. L.; Duncan, R. A.;
   Gary, D. E.; Gergely, T. E.; Harrison, R. A.; Howard, R. A.; Illing,
   R. M. E.; Jackson, B. V.; Kahler, S. W.; Kopp, K.; Low, B. C.; Lantos,
   P.; Phillips, K. J. H.; Poletto, G.; Sheeley, N. R., Jr.; Steward,
   R. T.; Svestka, Z.; Waggett, P. W.; Wu, S. T.
1986epos.conf6.366H    Altcode: 1986epos.confF.366H
  No abstract at ADS

---------------------------------------------------------
Title: Book-Review - Progress in Solar Physics
Authors: de Jager, C.; Svestka, Z.
1986S&T....72R.479D    Altcode:
  No abstract at ADS

---------------------------------------------------------
Title: Flaring Arches in Hα and X-Rays
Authors: Martin, S. F.; Svestka, Z.
1986BAAS...18Q.898M    Altcode:
  No abstract at ADS

---------------------------------------------------------
Title: X-ray imaging of flare loops and coronal arches
Authors: Svestka, Z.
1986sfcp.nasa...41S    Altcode:
  HXIS (Hard X-ray Imaging Spectrometer) results related to
  preflare, flare-decay, and post-flare phases in the solar corona
  are summarized. Particularly discussed are miniflares, long-lived
  X-ray enhancements along filament channels, flare precursors (some
  signifying the flare position, others possibly related to the onset
  of mass ejections), growth of post-flare loops, images of sites of
  field-line reconnections late in the flare development, giant post-flare
  coronal arches with energy contents comparable to coronal transients,
  and hot loops interconnecting active regions. The extremely low HXIS
  background, in particular, made it possible to discover many new,
  previously unknown features in the solar corona. Also emphasized are
  some problems that have appeared during the evaluation of HXIS data,
  for the benefit of those who plan future hard X-ray imaging experiments.

---------------------------------------------------------
Title: Coronal interconnection of two active regions observed in
    3.5 8.0 keV X-rays
Authors: Farnik, F.; van Beek, H. F.; Svestka, Z.
1986SoPh..104..321F    Altcode:
  Using HXIS data, we have studied the further development of the coronal
  arch extending towards the SE above active region No. 17255 in November
  1980. The arch, studied originally by Švestka (1984) disappeared
  on 10 November (after pronounced revival), but since 9 November HXIS
  revealed another arch-like structure towards the SW. We have studied
  the development of this new structure which appeared to be most likely
  an arch interconnecting AR 17255 with AR 17251, located nearly 30° to
  the west. This interconnection revived many times during the following
  days with intensity varying with the activity in both active regions. We
  have estimated the physical characteristics in this coronal structure
  and compared them with observations of interconnecting loops made
  at lower energies by Skylab in 1973. The temperature (maximum values
  7.5-14 × 10<SUP>6</SUP> K) and the density (1.1-5.0 × 10<SUP>9</SUP>
  cm<SUP>−3</SUP>) are found to be higher than in the Skylab loops
  (a result that could be expected because the HXIS energy range was
  harder than that of Skylab) and similar to the values deduced for
  the earlier arch system extending to the SE. However, much shorter
  decay times of the brightness variations indicate the presence of
  conduction in contrast to the SE arch in which conduction was clearly
  inhibited. This supports the assumption that the SE and SW coronal
  structures were two different phenomena.

---------------------------------------------------------
Title: Images of Post-Flare Coronal Structures in X-Rays
Authors: Svestka, Z.; Hick, P.
1986SoPh..104..187S    Altcode:
  This is an extended abstract of several papers mentioned in the
  references describing extensive coronal structures related to radio
  continua and imaged in &gt; 3.5 keV X-rays.

---------------------------------------------------------
Title: Editorial
Authors: de Jager, Cornelis; Švestka, Zdeněk
1986SoPh..107..200D    Altcode: 1987SoPh..107..200D
  No abstract at ADS

---------------------------------------------------------
Title: Coronal mass ejection associated with the stationary post-flare
    arch of 21 22 May 1980
Authors: McCabe, Marie K.; Švestka, Zdeněk F.; Howard, Russell A.;
   Jackson, Bernard V.; Sheeley, Neil R.
1986SoPh..103..399M    Altcode:
  By using a combination of X-ray (HXIS), Hα (Haleakala), white-light
  corona (Solwind), and zodiacal light (Helios) images on 21-22 May, 1980
  we demonstrate, and try to explain, the co-existence of a coronal mass
  ejection with a stationary post-flare coronal arch. The mass ejection
  was seen, both by Solwind and Helios, in prolongation of the path of
  a powerful spray, whereas the active region filament did not erupt. A
  tentative comparison is made with other occurrences of stationary,
  or quasi-stationary post-flare coronal arches.

---------------------------------------------------------
Title: Observations of chromospheric flare dynamics at the next
    solar maximum specific recommendations of the Chromospheric Flare
    Dynamics Group.
Authors: Canfield, R. C.; Gaizauskas, V.; Kurokawa, H.; Martin, S. F.;
   Svestka, Z.
1986lasf.conf..489C    Altcode:
  No abstract at ADS

---------------------------------------------------------
Title: White light flares and atmospheric modeling (Working Group
    report).
Authors: Machado, M. E.; Avrett, E. H.; Falciani, R.; Fang, C.;
   Gesztelyi, L.; Henoux, J. -C.; Hiei, E.; Neidig, D. F.; Rust, D. M.;
   Sotirovski, P.; Svestka, Z.; Zirin, H.
1986lasf.conf..483M    Altcode:
  The authors give a short summary of their discussions, and a set
  of recommendations which may help in the study of white light flare
  emission processes.

---------------------------------------------------------
Title: Coronal mass ejections and coronal structures.
Authors: Hildner, E.; Bassi, J.; Bougeret, J. L.; Duncan, R. A.;
   Gary, D. E.; Gergely, T. E.; Harrison, R. A.; Howard, R. A.; Illing,
   R. M. E.; Jackson, B. V.; Kahler, S. W.; Kopp, K.; Low, B. C.; Lantos,
   P.; Phillips, K. J. H.; Poletto, G.; Sheeley, N. R., Jr.; Stewart,
   R. T.; Svestka, Z.; Waggett, P. W.; Wu, S. T.
1986NASCP2439....6H    Altcode:
  Contents: 1. Introduction. 2. Observations. 3. Initiation of
  coronal mass ejections - observations. 4. Modelling of coronal mass
  ejections and post-flare arches. 5. Interplanetary effects of coronal
  mass ejections. 6. The slowly varying corona near solar activity
  maximum. 7. Summary.

---------------------------------------------------------
Title: X-ray imaging of flare loops and coronal arches.
Authors: Svestka, Z.
1986NASCP2421...41S    Altcode:
  This paper summarizes HXIS results related to preflare, flare-decay,
  and post-flare phases in the solar corona. Particularly discussed are
  miniflares, long-lived X-ray enhancements along filament channels, flare
  precursors (some signifying the flare position, others possibly related
  to the onset of mass ejections), growth of post-flare loops, images of
  sites of field-line reconnections late in the flare development, giant
  post-flare coronal arches with energy contents comparable to coronal
  transients, and hot loops interconnecting active regions. The extremely
  low HXIS background, in particular, made it possible to discover many
  new, previously unknown features in the solar corona. Also emphasized
  are some problems that have appeared during the evaluation of HXIS data,
  for the benefit of those who plan future hard X-ray imaging experiments.

---------------------------------------------------------
Title: The physics of solar flares. Proceedings of Symposium 5 of
    the COSPARTwenty-sixth Plenary Meeting held in Toulouse, France,
    30th June - 11th July 1986.
Authors: de Jager, C.; Svestka, Z.
1986AdSpR...6f....D    Altcode: 1986AdSpR...6.....D
  Observations and theoretical models of solar-flare phenomena
  are discussed in reviews and reports presented at the
  symposium formally marking the end of the international
  Solar-Maximum-Year/Solar-Maximum-Analysis project. Topics examined
  include flare buildup, precursors, and onset; the impulsive phase;
  the gradual phase; and coronal and interplanetary phenomena.

---------------------------------------------------------
Title: On the varieties of solar flares.
Authors: Svestka, Zdenek
1986lasf.conf..332S    Altcode: 1986lasf.symp..332S
  An attempt is made to classify flares starting with two axiomatic
  assumptions: (1) that a flare is a short-lived release of energy
  in consequence of a rearrangement of the magnetic structure, and
  (2) the mode of energy release is a reconnection of magnetic field
  lines. Somewhat surprisingly, in spite of the enormous diversity
  of the flare phenomena, two classes are derived: dynamic flares and
  confined flares, where the confined flares may be subdivided in two
  subclasses. All the other varieties may be due to differences in
  the boundary conditions of the flare process. The paper discusses
  the various factors which cause the varieties in flares, and the
  association of the two basic types of flares with different kinds of
  radiation and with othere active phenomena on the Sun.

---------------------------------------------------------
Title: Flare build-up study summary
Authors: Gaizauskas, V.; Svestka, Z.
1986AdSpR...6f...5G    Altcode: 1986AdSpR...6....5G
  No abstract at ADS

---------------------------------------------------------
Title: Progress in solar physics : review papers invited to celebrate
    the centennial volume of Solar physics
Authors: de Jager, Cornelis; Svestka, Zdenek
1986pspr.book.....D    Altcode: 1986QB521.6.P76....
  No abstract at ADS

---------------------------------------------------------
Title: A dynamic flare with anomalously dense flare loops
Authors: Svestka, Z.; Fontenla, J. M.; Machado, M. E.; Martin, S. F.;
   Neidig, D. F.; Poletto, G.
1986AdSpR...6f.253S    Altcode: 1986AdSpR...6..253S
  The dynamic flare of 6 November 1980 (max. ~ 15:26 UT) developed a
  rich system of growing loops which could be followed in Hα for 1.5
  hours. Throughout the flare, these loops, near the limb, were seen in
  emission against the disk. Theoretical computations of b-values for
  a hydrogen atom reveal that this requires electron densities in the
  loops to be close to 10<SUP>12</SUP> cm<SUP>-3</SUP>. From measured
  widths of higher Balmer lines the density at the loops of the loops
  was found to be 4 × 10<SUP>12</SUP> cm<SUP>-3</SUP> if no non-thermal
  motions were present. It is now general knowledge that flare loops
  are initially observed in X-rays and become visible in Hα only after
  cooling. For such a high density a loop would cool through radiation
  from 10<SUP>7</SUP> K to 10<SUP>4</SUP> K within a few minutes so that
  the dense Hα loops should have heights very close to the heights of
  the X-ray loops. This, however, contradicts the observations obtained by
  the HXIS and FCS instruments on board SMM which show the X-ray loops at
  much higher altitudes than the loops in Hα. Therefore, the density must
  have been significantly smaller when the loops were formed and the flare
  loops were apparently both shrinking and becoming denser while cooling.

---------------------------------------------------------
Title: The stationary post-flare arch of May 21/22, 1980
Authors: Hick, P.; Svestka, Z.
1985SoPh..102..147H    Altcode:
  On May 21/22, 1980 the Hard X-Ray Imaging Spectrometer aboard the
  SMM imaged an extensive coronal structure after the occurrence of a
  two-ribbon flare on May 21, 20:50 UT. The structure was observed from
  22:20 UT on May 21 until its disappearence at 09:00 UT on May 22.

---------------------------------------------------------
Title: 21 May 1980 flare review
Authors: de Jager, C.; Svestka, Z.
1985SoPh..100..435D    Altcode:
  A review is given of observations and theories relevant to the
  solar flare of 21 May, 1980, 20 ∶ 50 UT, the best studied flare
  on record. For more than 30 hr before the flare there was filament
  activation and plasma heating to above 10 MK. A flare precursor
  was present ≥6 min before the flare onset. The flare started with
  filament activation (20 ∶ 50 UT), followed by thick-target heating
  of two footpoints and subsequent ablation and convective evaporation
  involving energies of 1 to 2 × 10<SUP>31</SUP> erg. Coronal explosions
  occurred at 20 ∶ 57 UT (possibly associated with a type-II burst)
  and at 21 ∶ 04 UT (associated with an Hα spray?). Post-flare loops
  were first seen at 20 ∶ 57 UT, and their upward motion is interpreted
  as a manifestation of successive field-line reconnections. A type-IV
  radio burst which later changed into a type-I noise storm was related
  to a giant coronal arch located just below the radio noise storm
  region. Some implications and difficulties these observations present
  to current flare theories are mentioned.

---------------------------------------------------------
Title: Hard X-ray images of possible reconnection in the flare of
    21 May, 1980
Authors: Svestka, Z.; Poletto, G.
1985SoPh...97..113S    Altcode:
  An analysis of the growth of X-ray loops in the flare of 21 May, 1980,
  observed by HXIS on board SMM spacecraft, has been carried out with
  high time resolution in six energy channels from 3.5 to 30 keV. This
  analysis has revealed that the tops of the loops stay for minutes at a
  given altitude before, quite abruptly, other loop tops begin to appear
  above them. One of the jumps in altitude, from ∼27 000 to ∼45
  000 km if the loops extended radially, which occurred quite late in
  the flare development, is studied in detail. The fact that the tops,
  of higher loops were first seen in the 22-30 keV energy channel, and
  only minutes later at lower energies, suggests a new release of energy
  in a very small volume high in the corona. An initial temperature of
  at least 50 × 10<SUP>6</SUP> K is indicated by the data, inside a
  volume which may not exceed a few hundred km in diameter. A magnetic
  reconnection of previously distended field lines appears to be a likely
  candidate for the observed phenomenon.

---------------------------------------------------------
Title: Images of a Major Compact Flare in Hard X-rays and H-alpha
Authors: Svestka, Z.; Martin, S. F.
1985BAAS...17..628S    Altcode:
  No abstract at ADS

---------------------------------------------------------
Title: Book-Review - Astronomy and Astrophysics Abstracts
Authors: Bohme, S.; Svestka, Z.
1984SoPh...94..427B    Altcode:
  No abstract at ADS

---------------------------------------------------------
Title: Book reviews
Authors: Valníček, B.; Švestka, Zdeněk
1984SoPh...94..427V    Altcode:
  No abstract at ADS

---------------------------------------------------------
Title: Revivals of a Coronal Arch
Authors: Svestka, Z.
1984SoPh...94..171S    Altcode:
  The giant post-flare arch of 6 November 1980 revived 11 hr and 25 hr
  after its formation. Both these revivals were caused by two-ribbon
  flares with growing systems of loops. The first two brightenings of
  the arch were homologous events with brightness maxima moving upwards
  through the corona with rather constant speed; during all three
  brightenings the arch showed a velocity pattern with two components:
  a slow one (8-12 km<SUP>−1</SUP>), related to the moving maxima of
  brightness, and a fast one (∼ 35 km s<SUP>−1</SUP>), the source
  of which is unknown.

---------------------------------------------------------
Title: Hα and Hard X-Ray Development in Two-Ribbon Flares
Authors: Dwivedi, B. N.; Hudson, H. S.; Kane, S. R.; Svestka, Z.
1984SoPh...90..331D    Altcode:
  Morphological features of two-ribbon flares have been studied, using
  simultaneous ISEE-3 hard X-ray records and high-resolution Big Bear
  Hα movies for more than 20 events. Long-lasting and complex hard
  X-ray bursts are almost invariably found associated with flares of the
  two-ribbon type. We find at least three events, namely March 31, 1979,
  April 10, 1980, and July 1, 1980, where the occurrence of individual
  spikes in hard X-ray radiation coincides with suddenly enhanced Hα
  emission covering the sunspot penumbra. There definitely exist important
  (≥ 1B) two-ribbon Hα flares without significant hard X-ray emission.

---------------------------------------------------------
Title: Imaging of reconnection processes in hard X-rays
Authors: Švestka, Zdenek; Poletto, Giannina
1984AdSpR...4g.287S    Altcode: 1984AdSpR...4Q.287S
  The Hard X-ray Spectrometer aboard the SMM detected several events of
  energy release late in the development of two-ribbon flares. One such
  event, at 21:12 UT on 21 May, 1980 (~ 20 min after the flare onset and
  15 min after the peak of the impulsive phase) is studied in detail. The
  site of new brightening first became visible in hard X-rays (&gt; 22
  keV) and only afterwards showed up at lower energies. It was clearly
  located high in the corona so that one can identify it with energy
  release at the tops of newly formed post-flare loops. Thus, if the
  Kopp and Pneuman model of the loop formation is adopted, we may have
  imaged here a reconnection process in the solar corona. An attempt is
  made to estimate physical parameters at the reconnection site.

---------------------------------------------------------
Title: Post-flare thermal waves in the solar corona
Authors: Svestka, Z.
1984AdSpR...4g.179S    Altcode: 1984AdSpR...4..179S
  While imaging giant post-flare arches in the solar corona, the Hard
  X-Ray Spectrometer aboard the SMM detected thermal disturbances
  propagating through the corona after two-ribbon flares. The speed
  of propagation is close to, or below, 10 km s<SUP>-1</SUP>, and no
  obvious time-variation of the speed is indicated in the HXIS data. For
  subsequent two-ribbon flares in the same active region, these thermal
  disturbances (waves) exhibit highly homologous properties; thus the
  waves appear to propagate through preexisting arches formed after
  earlier flares. Temperatures of &gt; 20 × 10<SUP>6</SUP> K have been
  detected in these moving phenomena. We suggest that we see here in
  X-rays upper products of the consecutive reconnections which create
  the post-flare loops below. Temperature maps in fine field of view
  of HXIS offer now a new possibility to detect postflare arches in the
  corona built during two-ribbon flares.

---------------------------------------------------------
Title: Large post-flare arch-like structures in the solar corona
Authors: Svestka, Z.
1984MmSAI..55..725S    Altcode:
  Hard (3.5-10-keV) X-ray observations of large archlike structures in the
  solar corona, obtained with the SMM HXIS after two-ribbon flares on May
  22 and November 6, 1980 (Svestka et al., 1982), are presented in maps
  and graphs along with Culgoora radioheliograph, Bonn radio-telescope,
  Nancay radio-interferometer, and GOES-2 X-ray data and analyzed using a
  theoretical model of postflare loop formation by sequential reconnection
  of distended field lines (Kopp and Pneuman, 1976). Stationary or
  slowly expanding arches of temperature 2 x 10 to the 7th K or more,
  with thermal disturbances propagating upward at about 10 km/s, are
  observed in association with type I radio noise storms for periods of
  10 h or more. The quasi-periodic X-ray and radio flux variations seen
  above and below the arches in the later stages are attributed to the
  transition from a system of interconnected loops along the neutral
  line to groups of isolated plasmoids with repetitive instabilities.

---------------------------------------------------------
Title: Enhanced X-Ray Emission above 3.5-KEV in Active Regions in
    the Absence of Flares
Authors: Schadee, A.; de Jager, C.; Svestka, Z.
1983SoPh...89..287S    Altcode:
  We demonstrate that even in the absence of flares there are very
  often volumes of hot plasma in the corona above active regions with
  temperatures in excess of 10 million degrees. Characteristics of
  this hot plasma and its time variations seem to be different in
  active regions of different phase of development. These hot plasma
  regions are sources of very weak, but clearly recognizable, X-ray
  emission above 3.5 keV. Long-lived X-ray brightenings, 10<SUP>4</SUP>
  times weaker than a flare, but lasting up to 10 hr occur predominantly
  along the H<SUB>∥</SUB> = 0 line, apparently low in the corona. After
  major flares, long-lived X-ray emission is also radiated from tops of
  arches extending high into the corona. Some other long-lived sources,
  far from the H<SUB>∥</SUB> = 0 line, may be associated with newly
  emerging flux. Short-lived X-ray sources, with fluxes ranging from
  subflare levels to 10<SUP>−3</SUP> times the flare flux, last for
  2 to more than 30 min and are probably microflares. They seem to be
  most frequent in growing young active regions and appear often in
  areas with newly emerging flux.

---------------------------------------------------------
Title: Radio, X-ray, and optical observations of the flare of June
    13, 1980, at 6<SUP>h</SUP>22<SUP>m</SUP> UT
Authors: Kattenberg, A.; Allaart, M.; de Jager, C.; Schadee, A.;
   Schrijver, J.; Shibasaki, K.; Švestka, Z.; van Tend, W.
1983SoPh...88..315K    Altcode:
  A subflare of importance Sf was observed on June 13, 1980 simultaneously
  by instruments aboard the Solar Maximum Mission (SMM) and various
  ground based observatories. We describe and compare different kinds
  of observations, with emphasis on the Hard X-Ray Imaging Spectrometer
  (HXIS) images and spectra, and on the one-dimensional microwave images
  with high time and spatial resolution, obtained with the Westerbork
  Synthesis Radio Telescope (WSRT). The fast electrons causing the X-ray
  and microwave impulsive bursts had a common acceleration source, but the
  burst were produced at the opposite footpoints of the loops involved,
  with microwaves emitted near to a sunspot penumbra. The flare (of a
  `compact' type) was probably triggered by an emerging flux, and two
  possible interpretations of this process are briefly discussed.

---------------------------------------------------------
Title: Transient brightenings of interconnecting
    loops. III. Interpretation.
Authors: Spicer, D. S.; Svestka, Z.
1983SoPh...87..271S    Altcode:
  We present two alternative interpretations of the sudden X-ray
  brightenings observed in loops that interconnect active regions. A
  fast tearing mode may be excited in those newly formed interconnecting
  loops within which sufficient magnetic free energy is stored to drive
  the mode. Alternatively anomalous Joule heating driven by an inductive
  electric field parallel to the magnetic field varying on a time scale
  of order of a minute may cause the brightenings. We argue that it is
  plausible that the fast tearing mode may be the cause of brightenings
  in the young newly formed interconnecting loops, whereas the anomalous
  Joule heating might occur in old loop connections when an external
  disturbance propagates through them.

---------------------------------------------------------
Title: POST Flare Coronal Arches
Authors: Svestka, Z.
1983SSRv...35..259S    Altcode:
  The Hard X-ray Imaging Spectrometer aboard the SMM detected gigantic
  arches in the corona which are formed or, if preexisting, become
  excited after major two-ribbon flares. They are seen in 3.5 8 keV
  X-rays and extend along the H <SUB>∥</SUB> = 0 line to altitudes
  between 10<SUP>5</SUP> and 2 × 10<SUP>5</SUP> km. These arches are
  stationary and form the base of a stationary type I radio noise storm
  initiated by the flare. They are visible in X-rays for ten hours or
  more and may be revived, in temperature, density, and brightness, if
  another two-ribbon flare appears below them. We suggest that they are
  built-up through reconnection process during the flare from the upper
  reconnected loops in the Kopp and Pneuman model. These loops become
  interconnected along the H <SUB>∥</SUB> = 0 line in consequence
  of great shear of the reconnecting loops. Obviously, the coronal
  transient associated with such flares must be either accomplished prior
  to the formation of the arch, or it must be formed through a process
  different from the Anzer-Kopp-Pneuman mechanism. Striking brightness
  variations occur quasi-periodically in the corona below and above
  the arch a few hours after the flare. These variations are seen at
  about the same time in soft X-rays, hard X-rays, and on centimeter
  microwaves in the low corona, as well as at metric waves in the type
  I noise-storm region. In spite of their flare-like intensity, however,
  the variations have little response in the transition layer (O v line)
  and no response at all in the chromosphere (Hα). We suggest that
  these semi-periodic brightenings are due to repetitive acceleration
  processes in plasmoids that encircle the arch perpendicular to the H
  <SUB>∥</SUB> = 0 line from the low corona through the noise storm
  region, being completely detached from the lower atmospheric layers.

---------------------------------------------------------
Title: Pre-Flare and Post-Flare X-Ray Variations in Active Regions
Authors: Svestka, Z.; Schadee, A.
1983SoPh...86..267S    Altcode:
  Extremely low background noise of the HXIS experiment aboard the SMM
  made it possible to detect &gt; 3.5 keV X-ray emissions from non-flaring
  active regions which are 10<SUP>3</SUP>-10<SUP>4</SUP> times weaker than
  the X-ray flux from flares. Short-lived X-ray bursts and long-lived
  X-ray enhancements of various intensities seem to characterize active
  regions in different phases of their development. After major two-ribbon
  flares, giant X-ray arches are seen in the corona, slowly decaying for
  many hours after the flare end. Associated with these arches appear
  to be quasi-periodic flare-like variations of purely coronal nature.

---------------------------------------------------------
Title: Purely Coronal Flare-Like Variations
Authors: Svestka, Z.; Schrijver, J.; Somov, B.; Dennis, B. R.;
   Woodgate, B. E.; Fuerst, E.; Hirth, W.; Klein, L.; Raoult, A.
1983SoPh...85..313S    Altcode:
  A detailed study of the quasi-periodical post-flare variations on
  November 6, 1980 in X-rays, UV lines, microwaves, and metric waves
  confirms that these variations were predominantly thermal phenomena
  and occurred solely in the corona. Only the short-lived impulsive
  components that preceded all or most of the individual variations
  were of non-thermal character and penetrated down to the transition
  layer. The chromosphere (in Hα) did not participate in any part of
  these events, in contrast to a flare that appeared at the same place a
  few hours later. However, the X-ray emission of these variations was
  so strong that the transition layer and the chromosphere definitely
  should have been enhanced through heat conduction along the magnetic
  field lines. The expected heat flux at the top of the chromosphere
  coming from some of these coronal brightenings was 60-80% of the flux
  expected in the flare at 17:26 which gave rise to a 2B flare in Hα
  (Figure 8). Therefore, we suggest that the variations were produced in
  a coronal plasmoid with closed field lines completely detached from the
  lower atmospheric layers (Figure 9b). We also give reasons why such a
  detached plasmoid can be expected to be formded in the very late phase
  (some 4-5 hr after the onset) of a major two-ribbon flare.

---------------------------------------------------------
Title: The Queen's Flare - its Structure and Development - Precursors
    Pre-Flare Brightenings and Aftermaths
Authors: de Jager, Cornelis; Machado, Marcos E.; Schadee, Aert;
   Strong, Keith T.; Švestka, Zdeněk; Woodgate, Bruce E.; van Tend, W.
1983SoPh...84..205D    Altcode:
  We continue previous research on the limb flare of 30 April, 1980, 20:20
  UT, observed in X-rays by several instruments aboard the Solar Maximum
  Mission (SMM). It is shown quantitatively that the flare originated in
  an emerging magnetically confined kernel (diameter ∼ 20″) which
  existed for about ten to fifteen minutes, and from which energetic
  electrons streamed, in at least two injections, into a previously
  existing complicated magnetic loop system thus forming a less bright but
  extended and long-lived tongue. The tongue had a length of ∼ 35 000 km
  and lasted ∼ 90 min in X-rays (∼ 10 keV); at lower energies (∼ 0.7
  keV) it was larger (∼ 80 000 km) and lasted longer. The total number
  of energetic electrons (≈ 10<SUP>37</SUP>) initially present in the
  kernel is of the same order as the number present in the tongue after
  the kernel's decline. This gives evidence that the energetic electrons
  in the tongue originated mainly in the kernel. The electron number
  densities in the kernel and tongue at maximum brightness were ∼ 4.5
  × 10<SUP>11</SUP> and ∼ 1 × 10<SUP>11</SUP> cm<SUP>#X2212;3</SUP>,
  respectively. During the first eight minutes of its existence the tongue
  was hotter than the kernel, but it cooled off gradually. Its decline in
  intensity and temperature was exponential; energy was lost by radiation
  and by conduction through the footpoints of the loop system. These
  footpoints have a cross-section of only ∼ 3 × 10<SUP>6</SUP>
  km<SUP>2</SUP>. This small value, as well as photographs in a CIV UV
  emission line, suggests a highly filamentary structure of the system;
  this is further supported by the finding that the tongue had a `filling
  factor' of ∼ 10<SUP>#X2212;2</SUP>. Several faint X-ray brightenings
  (≲ 0.005 of the flare's maximum intensity) were observed at various
  locations along the solar limb for several hours before and after the
  flare. At ∼ 30 min before the flare's onset a faint (≲ 0.02) flare
  precursor occurred, coinciding in place and shape with the flare. First
  the kernel precursor was brightest but the tongue precursor increased
  continuously in brightness and was the brightest part of the precursor
  some 10-15 min after the first visibility of the kernel precursor,
  until the start of the main flare. This suggests (weak) continuous
  electron acceleration in the tongue during a period of at least 30
  min. The main flare was caused by strong emergence of magnetic field
  followed by two consecutive field line reconnections and accelerations
  in a small loop system, causing footpoint heating. Subsequently plasma
  streamed (convectively) into a pre-existing system of larger loops,
  forming the tongue.

---------------------------------------------------------
Title: 3.5 keV X-ray Emission in Absence of Flares
Authors: Schadee, A.; de Jager, C.; Svestka, Z.
1983BAAS...15R.704S    Altcode:
  No abstract at ADS

---------------------------------------------------------
Title: Revival of a Coronal Arch
Authors: Svestka, Z.
1983BAAS...15..714S    Altcode:
  No abstract at ADS

---------------------------------------------------------
Title: Particle acceleration in two-ribbon flares.
Authors: Švestka, Z.
1983POEM...14...69S    Altcode:
  The author points out the basic differences between compact and
  two-ribbon flares, and discusses observations indicating particle
  acceleration during a long-enduring reconnection process in the
  two-ribbon flares.

---------------------------------------------------------
Title: Particle acceleration in two-ribbon flares
Authors: Svestka, Z.
1983ebro.conf...69S    Altcode:
  Particle acceleration during a long reconnection process in two-ribbon
  flares is discussed. The evolution in the understanding of solar
  flares is summarized, pointing out the contributions of the Skylab
  mission and other satellite observation missions. A model of a
  two-ribbon flare is described. Particle acceleration is associated
  with magnetic reconnection when new loops are formed. Particles are
  trapped in the loops and produce the hard X-ray, H alpha and white light
  emission. According to the model, particle acceleration in two-ribbon
  flares may last for hours, and in filament disruptions, in particular
  along the boundaries of growing coronal holes, non negligible particle
  fluxes in space may be produced.

---------------------------------------------------------
Title: Unusual coronal activity following the flare of 6 November 1980
Authors: Švestka, Z.; Dennis, B. R.; Pick, M.; Raoult, A.; Rapley,
   C. G.; Stewart, R. T.; Woodgate, B. E.
1982SoPh...80..143S    Altcode:
  For almost 30 hr after the major (gamma-ray) two-ribbon flare on 6
  November 1980, 03:30 UT, the Hard X-Ray Imaging Spectrometer (HXIS)
  aboard the SMM satellite imaged in &gt; 3.5 keV X-rays a gigantic
  arch extending above the active region over the limb. Like a similar
  configuration on 22 May 1980, this arch formed the lowest part of a
  stationary post-flare radio noise storm recorded at metric wavelengths
  at Nançay and Culgoora. 6.5 hr after the flare a coronal region below
  the arch started quasi-periodic pulsations in X-ray brightness, observed
  by several SMM instruments. These brightness variations had no response
  in the chromosphere (Hα), very little in the transition layer (O v),
  but they clearly correlated with similar variations in brightness at
  169 MHz. There were 13 pulses of this kind, with apparent periodicity
  of about 20 min, until another flare occurred in the active region at
  ∼ 15:00 UT. All the brightenings appeared within a localized area of
  about 30000 km<SUP>2</SUP> in the northern part of the active region,
  but they definitely did not occur all at the same place.

---------------------------------------------------------
Title: Study of the Post-Flare Loops on 1973JUL29 - Part Four -
    Revision of T and NE Values and Comparison with the Flare of 1980MAY21
Authors: Švestka, Z.; Dodson-Prince, H. W.; Martin, S. F.; Mohler,
   O. C.; Moore, R. L.; Nolte, J. T.; Petrasso, R. D.
1982SoPh...78..271S    Altcode:
  We present revised values of temperature and density for the flare
  loops of 29 July 1973 and compare the revised parameters with those
  obtained aboard the SMM for the two-ribbon flare of 21 May 1980. The 21
  May flare occurred in a developed sunspot group; the 29 July event was a
  spotless two-ribbon flare. We find that the loops in the spotless flare
  extended higher (by a factor of 1.4-2.2), were less dense (by a factor
  of 5 or more in the first hour of development), were generally hotter,
  and the whole loop system decayed much slower than in the spotted flare
  (i.e. staying at higher temperature for a longer time). We also align
  the hot X-ray loops of the 29 July flare with the bright Hα ribbons
  and show that the Hα emission is brightest at the places where the
  spatial density of the hot elementary loops is enhanced.

---------------------------------------------------------
Title: Observations of a POST Flare Radio Burst in X-Rays
Authors: Svestka, Z.; Hoyng, P.; van Tend, W.; Boelee, A.; de Jager,
   C.; Stewart, R. T.; Acton, L. W.; Bruner, E. C.; Gabriel, A. H.;
   Rapley, C. G.; de Jager, C.; LaFleur, H.; Nelson, G.; Simnett, G. M.;
   van Beek, H. F.; Wagner, W. J.
1982SoPh...75..305S    Altcode:
  More than six hours after the two-ribbon flare of 21 May 1980, the
  hard X-ray spectrometer aboard the SMM imaged an extensive arch above
  the flare region which proved to be the lowest part of a stationary
  post-flare noise storm recorded at the same time at Culgoora. The X-ray
  arch extended over 3 or more arc minutes to a projected distance of
  95 000 km, and its real altitude was most probably between 110 000
  and 180 000 km. The mean electron density in the cloud was close to
  10<SUP>9</SUP> cm<SUP>−3</SUP> and its temperature stayed for many
  hours at a fairly constant value of about 6.5 × 10<SUP>6</SUP> K. The
  bent crystal spectrometer aboard the SMM confirms that the arch emission
  was basically thermal. Variations in brightness and energy spectrum at
  one of the supposed footpoints of the arch seem to correlate in time
  with radio brightness suggesting that suprathermal particles from
  the radio noise regions dumped in variable quantities into the low
  corona and transition layer; these particles may have contributed to
  the population of the arch, after being trapped and thermalized. The
  arch extended along the H<SUB>∥</SUB> = 0 line thus apparently
  hindering any upward movement of the upper loops reconnected in the
  flare process. There is evidence from Culgoora that this obstacle may
  have been present above the flare since 15-30 min after its onset.

---------------------------------------------------------
Title: Solar Maximum Year; Proceedings of the Symposium, Ottawa,
    Canada, May 16-June 2, 1982
Authors: Svestka, Z.; Rust, D. M.; Dryer, M.
1982AdSpR...2k....S    Altcode: 1982AdSpR...2.....S
  Results of research conducted during the Solar Maximum Year from
  August 1979 to through February 1981 are presented, focusing on flare
  build-up, energy release in flares, and travelling interplanetary
  phenomena. Topics examined include the relation of solar flares to the
  evolution and proper motions of magnetic fields, pre-flare heating of
  filaments, mass motions in a quiescent filament, multiple wavelength
  observations of flaring active regions, energy transfer in solar flares,
  direct evidence for chromosphere evaporation in a well-observed compact
  flare, physics of the impulsive phase of solar flares, and the analysis
  of ultra-fast fine structures of microwave bursts. Also considered
  are the effects of electron-cyclotron masers during flares, high
  energy particle acceleration in flares, particle charge interchange
  during acceleration in flare regions, diamagnetic aspects of the
  coronal transient phenomenon, particle acceleration by coronal and
  interplanetary shock waves, and the propagation of energetic particles
  in the solar wind. For individual items see A83-35202 to A83-35235

---------------------------------------------------------
Title: Transient Brightenings of Interconnecting Loops - Part Two -
    Dynamics of the Brightened Loops
Authors: Svestka, Z.; Howard, R.
1981SoPh...71..349S    Altcode:
  We discuss three different kinds of dynamic events related to
  interconnecting loops observed in soft X-rays aboard Skylab: (1)
  A newly born transequatorial loop that was either emerging from
  subphotospheric layers or gradually filled in with hot plasma. (2)
  Large-scale twists of interconnecting loops which never relax, and
  often only form, after the loop brightenings. (3) Three events where
  the loop that later interconnected two active regions had been visible
  long before one of the interconnecting regions was born. Several impacts
  this observation might have upon our understanding of the process of
  flux emergence are suggested.

---------------------------------------------------------
Title: Origin and Location of the Hard X-Ray Emission in a Two-Ribbon
    Flare
Authors: Hoyng, P.; Duijveman, A.; Machado, M. E.; Rust, D. M.;
   Svestka, Z.; Boelee, A.; de Jager, C.; Frost, K. T.; Lafleur, H.;
   Simnett, G. M.; van Beek, H. F.; Woodgate, B. E.
1981ApJ...246L.155H    Altcode:
  No abstract at ADS

---------------------------------------------------------
Title: On the outburst of flare activity of 26 November, 1973
Authors: Howard, R.; Svestka, Z.
1981SoPh...71...49H    Altcode:
  We draw attention of flare build-up observers to a strong 30 hour-long
  outburst of homologous flare activity and unusual growth and brightening
  of coronal loops, seen on Skylab. We suggest that these events might
  have been closely associated with newly emerging magnetic flux, in
  spite of the fact that the flux effects in Hα and EUV were first seen
  only late after the activity had started, and the flux emerged at the
  opposite end of the coronal loops from where the flares occurred.

---------------------------------------------------------
Title: Coronal Variations Imaged in 3.5 - 30 keV X-Rays
Authors: Svestka, Z.
1981BAAS...13..909S    Altcode:
  No abstract at ADS

---------------------------------------------------------
Title: Giant X-Ray Arches Associated with Post-Flare Radio Noise
    Storms
Authors: Svestka, Z.; Pick, M.; Rapley, C. G.; Stewart, R. T.;
   Woodgate, B.
1981BAAS...13..555S    Altcode:
  No abstract at ADS

---------------------------------------------------------
Title: X-Ray Observations of Two Different Systems of "Post Flare"
    Loops
Authors: Svestka, Z.; Dodson-Prince, H. W.; Mohler, O. C.; Martin,
   S. F.; Moore, R. L.; Nolte, J. T.; Petrasso, R. D.
1981BAAS...13R.542S    Altcode:
  No abstract at ADS

---------------------------------------------------------
Title: The limb flare of 1980 April 30 as seen by the hard X-ray
    imaging spectrometer
Authors: van Beek, H. F.; de Jager, C.; Schadee, A.; Svestka, Z.;
   Boelee, A.; Duijveman, A.; Galama, M.; Hoekstra, R.; Hoyng, P.; Fryer,
   R.; Simnett, G. M.; Imhof, J. P.; LaFleur, H.; Maseland, H. V. A. M.;
   Mels, W. M.; Schrijver, J.; van der Laan, J. J. M.; van Rens, P.; van
   Tend, W.; Werkhoven, F.; Willmore, A. P.; Wilson, J. W. G.; Machado,
   M. E.; Zandee, W.
1981ApJ...244L.157V    Altcode:
  X-ray imaging of the limb event of 1980 April 30 shows that the flaring
  involved two distinct components: a pointlike component, which was the
  source of the initial hard X-ray burst and an extensive tongue reaching
  some 30,000 km above the limb. The tongue had a higher temperature
  than the other parts of the structure and seemed to be enhanced by
  energetic electrons that derived their energy from the initial source.

---------------------------------------------------------
Title: Introduction
Authors: De Jager, Cornelis; Švestka, Zdeněk
1981SoPh...72D...7D    Altcode:
  No abstract at ADS

---------------------------------------------------------
Title: Book-Review - Astronomy and Astrophysics Abstracts V.25
    &amp; 26
Authors: Bohme, S.; Esser, U.; Fricke, W.; Svestka, Z.
1981SoPh...69..419B    Altcode:
  No abstract at ADS

---------------------------------------------------------
Title: Book review
Authors: Švestka, Z.
1981SoPh...69..419S    Altcode:
  No abstract at ADS

---------------------------------------------------------
Title: Structural development of the X-ray limb flare of 30 April 1980
Authors: de Jager, C.; Hoyng, P.; Lafleur, H.; Schadee, A.; Svestka,
   Z.; van Beek, H. F.; van Tend, W.; Fryer, R.; Simnett, G. M.
1981AdSpR...1m.251D    Altcode: 1981AdSpR...1..251D
  We describe the development of the limb flare of 30 April 1980, 20:20
  UT, as observed by the Hard X-ray Imaging Spectrometer (HXIS) aboard
  the Solar Maximum Mission (SMM). It consisted of a short-lived bright
  nucleus (FWHM &lt; 10,000 km), just inside the Sun's limb; a longer
  lasting tongue, extending to a height of ~ 30,000 km, and a more
  complicated feature, approximately situated at the Sun's limb. The
  tongue was a pre-existing magnetic structure that started emitting
  X-rays only a few seconds after the bright nucleus, and which had a
  slightly higher temperature than the nucleus; its X-ray emission may
  be caused by electrons escaped from the nucleus.

---------------------------------------------------------
Title: Solar maximum mission experiment: Early results of the hard
    X-ray imaging experiment
Authors: Boelee, A.; de Jager, C.; Duijveman, A.; Galama, M.; Hoekstra,
   R.; Hoyng, P.; Imhof, J. P.; Lafleur, H.; Maseland, H. V. A. M.; Mels,
   W. A.; Schadee, A.; Schrijver, J.; Svestka, Z.; van Beek, H. F.;
   van Rens, P.; van der Laan, J. J. M.; van Tend, W.; Werkhoven, F.;
   Wiersma, G.; Zandee, W.; Simnett, G. M.; Charlton, C. P.; Fryer, R.;
   Willmore, A. P.; Wilson, J. W. G.; Machado, M. E.
1981AdSpR...1m.255B    Altcode: 1981AdSpR...1R.255B
  We have selected four widely different flares from the early
  period of operations of the Hard X-Ray Imaging Spectrometer (HXIS)
  on SMM to illustrate the characteristic imaging properties of this
  experiment. For the small flare of April 4, 1980, we demonstrate the
  instrument's capability for locating a compact source. In the weak,
  but extensive, flare of April 6 we show how well the instrument can
  display spatial structure, and also the low level of the instrument
  background. In the 1B flare of April 7 we are able to locate positions
  of the X-ray emission in the soft and hard channels, and estimate
  the positional variations of the emission patches. Finally, in the IN
  flare of April 10, which produced the strongest hard X-ray burst we
  have seen so far, we repeat some of the studies made for the April 7
  event, and also demonstrate the capability of the HXIS instrument to
  study the development, with high time resolution, of individual 8”
  × 8” elements of the flare.

---------------------------------------------------------
Title: Flare observations
Authors: Svestka, Z.
1981sfmh.book...47S    Altcode:
  The solar flare represents a sudden release of energy in the atmospheric
  layers of the sun. In tens of seconds or a few minutes the temperature
  rises throughout the solar atmosphere, reaching its peak, often
  well above 10 million K, in the solar corona. Flare observations
  in the H-alpha light are considered along with chromospheric flare
  spectra, thermal flares in soft X-rays, impulsive hard X-ray and
  microwave bursts, energy transfer through the transition layer,
  metric radio bursts, flare ejecta, and the production and effects of
  high-energy particles in flares. Attention is given to the general
  characteristics of flares, flare emissions, flare classification,
  two-ribbon and compact flares, flare theory, flares in relation to
  magnetic fields, flare occurrence, flares in relation to velocity
  fields, flare-associated changes in the magnetic field, the EUV
  spectrum, the EUV flare morphology and density, and flare waves.

---------------------------------------------------------
Title: Structural development of the X-ray limb flare of 30 April
    1980.
Authors: de Jager, C.; Fryer, R.; Hoyng, P.; Lafleur, H.; Schadee,
   A.; Simnett, G. M.; Svestka, Z.; van Beek, H. F.; van Tend, W.
1981hea..conf..251D    Altcode:
  No abstract at ADS

---------------------------------------------------------
Title: Solar Maximum Mission experiment: early results of the hard
    X-ray imaging experiment.
Authors: Simnett, G. M.; Boelee, A.; Charlton, C. P.; de Jager, C.;
   Duijveman, A.; Fryer, R.; Galama, M.; Hoekstra, R.; Hoyng, P.; Imhof,
   J. P.; Lafleur, H.; Machado, M. E.; Maseland, H. V. A. M.; Mels,
   W. A.; Schadee, A.; Schrijver, J.; Svestka, Z.; van Beek, H. F.;
   van Rens, P.; van der Laan, J. J. M.; van Tend, W.; Werkhoven, F.;
   Wiersma, G.; Willmore, A. P.; Wilson, J. W. G.; Zandee, W.
1981hea..conf..255S    Altcode:
  No abstract at ADS

---------------------------------------------------------
Title: Hα and Hard X-Ray Development in Two-Ribbon Flares
Authors: Dwivedi, B. N.; Hudson, H. S.; Kane, S. R.; Svestka, Z.
1980BAAS...12..905D    Altcode:
  No abstract at ADS

---------------------------------------------------------
Title: A Study of the Impulsive Flares and Homologous Flares From
    AR2372 From April 6-13, Using Hard X-Ray Images
Authors: Simnett, G. M.; Machado, M.; Harrison, R. A.; Hoyng, P.;
   Lafleur, H.; Svestka, Z.; Vanbeek, H. F.
1980BAAS...12S.899S    Altcode:
  No abstract at ADS

---------------------------------------------------------
Title: The Solar Maximum Year and Related Space Experiments
Authors: Svestka, Z.; de Jager, C.
1980SSRv...26..317S    Altcode:
  The Solar Maximum Year is a world-wide cooperative project to gain
  more insight in certain aspects of solar flares. It consists of three
  sub-programs: The Flare Build-up Study (FBS), the Study of Energy
  Release from Flares (SERF), and the Study of Travelling Interplanetary
  Phenomena (STIP). These programs are described. We also describe space
  observations to be performed during SMY, particularly the Solar Maximum
  Mission Satellite.

---------------------------------------------------------
Title: Activated Solar Filaments and Flares
Authors: Svestka, Z.
1980RSPTA.297..575S    Altcode: 1980RSLPT.297..575S
  Activations and disruptions of dark Hα filaments are very common
  phenomena on the Sun. They precede the most powerful two-ribbon
  solar flares, but they also appear far from any active region
  without any chromospheric flaring. Therefore, until very recently,
  filament disruptions were considered as interesting, but physically
  insignificant, flare precursors. Only Skylab observations have shown
  that the filament disruptions actually represent one of the basic
  and most important mechanisms of solar activity. These observations
  have revealed (1) that many coronal transients originate in eruptive
  filaments without chromospheric flares, (2) that Bruzek's slow-mode
  waves originate in disrupted filaments and not in flares themselves,
  and (3) that many coronal X-ray enhancements outside active regions
  are also tops of newly formed loops, similar to the post-flare loops
  observed after filament disruptions in active regions. An interpretation
  of these data stems from Kopp &amp; Pneuman's theory of post-flare
  loops: the process that disrupts a filament opens the magnetic field
  and causes a greatly enhanced mass-flow along the field lines. The
  open field lines subsequently reconnect, starting from the bottom
  of the corona and proceeding upwards. This process can last for many
  hours. Hot loops are first seen in X-rays, later in extreme ultraviolet
  (e.u.v.) lines, and, after an appropriate cooling time, in Hα as the
  loop prominence systems. The visibility of loops depends on plasma
  density. Several observed properties of solar flares indicate that
  the primary acceleration occurs as the field lines reconnect. Thus
  the process of particle acceleration in two-ribbon flares can last
  for hours. Because reconnection is accomplished after essentially all
  filament disruptions, 'disparitions brusques' outside active regions
  should also accelerate particles.

---------------------------------------------------------
Title: The Dynamics of Brightened Interconnecting Loops
Authors: Howard, R.; Svestka, Z.
1980BAAS...12..519H    Altcode:
  No abstract at ADS

---------------------------------------------------------
Title: Particle acceleration in the process of eruptive opening and
    reconnection of magnetic fields
Authors: Svestka, Z.; Martin, S. F.; Kopp, R. A.
1980IAUS...91..217S    Altcode:
  No abstract at ADS

---------------------------------------------------------
Title: The thermal X-ray flare plasma
Authors: Moore, R.; McKenzie, D. L.; Svestka, Z.; Widing, K. G.; Dere,
   K. P.; Antiochos, S. K.; Dodson-Prince, H. W.; Hiei, E.; Krall, K. R.;
   Krieger, A. S.
1980sfsl.work..341M    Altcode: 1980sofl.symp..341M
  Following a review of current observational and theoretical knowledge
  of the approximately 10 to the 7th K plasma emitting the thermal soft
  X-ray bursts accompanying every H alpha solar flare, the fundamental
  physical problem of the plasma, namely the formation and evolution of
  the observed X-ray arches, is examined. Extensive Skylab observations
  of the thermal X-ray plasmas in two large flares, a large subflare and
  several compact subflares are analyzed to determine plasma physical
  properties, deduce the dominant physical processes governing the plasma
  and compare large and small flare characteristics. Results indicate
  the density of the thermal X-ray plasma to be higher than previously
  thought (from 10 to the 10th to 10 to the 12th/cu cm for large to
  small flares), cooling to occur radiatively as much as conductively,
  heating to continue into the decay phase of large flares, and the
  mass of the thermal X-ray plasma to be supplied primarily through
  chromospheric evaporation. Implications of the results for the basic
  flare mechanism are indicated.

---------------------------------------------------------
Title: Gibt es Cluster von Hellen Punkten?
Authors: Kittelberger, G.; Elwert, G.; Svestka, Z.
1980MitAG..50...96K    Altcode:
  No abstract at ADS

---------------------------------------------------------
Title: The needs for prediction and real-time monitoring for the
    flare build-up study
Authors: Svestka, Z.
1979stp.....2..322S    Altcode:
  Similarities between plasma instabilities occurring in
  the magnetospheric tail and in active regions on the Sun are
  discussed. Intense observations of the flare build-up processes on the
  Sun planned for May and June 1980 as a part of the Solar Maximum Year
  are described.

---------------------------------------------------------
Title: Slowly moving disturbances in the X-ray corona.
Authors: Rust, D. M.; Svestka, Z.
1979SoPh...63..279R    Altcode:
  Sequences of soft X-ray pictures, taken aboard Skylab between May
  and November, 1973, have made it possible to detect slowly moving
  disturbances originating in disrupted filaments and causing subsequent
  brightenings of distant coronal structures. With speeds decreasing
  from ∼400 km s<SUP>-1</SUP> shortly after the filament disruption to
  ∼10 km s<SUP>-1</SUP> four or five hours later, these disturbances
  appear to be identical with slow waves earlier inferred by Bruzek,
  Öhman, and Yajima from chromospheric observations.

---------------------------------------------------------
Title: Transient brightenings of interconnecting loops. Morphology
    of the sudden brightenings.
Authors: Svestka, Z.; Howard, R.
1979SoPh...63..297S    Altcode:
  We study sudden brightenings of coronal loops that interconnect
  active regions. Such brightenings often occur within one or two
  days after the birth of a new interconnecting loop, as well as
  in some old interconnections. The brightenings of young loops are
  obviously associated with the emergence of new magnetic flux near their
  footpoints, whereas some enhancements of old loops may be triggered by
  slowly moving disturbances propagating from other centers of activity. A
  few loop brightenings are associated with flares, but the loop does
  not brighten in consequence of energy supply from the flare. Both the
  flare and the loop brightening are independent consequences of one
  common agent, presumably newly emerging flux.

---------------------------------------------------------
Title: The birthplaces of active regions and X-ray bright points.
Authors: Howard, R.; Fritzova-Svestkova, L.; Svestka, Z.
1979SoPh...63..105H    Altcode:
  A comparison of soft X-ray pictures of the Sun (S-054 experiment of
  Skylab) with K-line spectroheliograms (Mount Wilson) shows that the
  X-ray bright points tend to emerge randomly throughout the Ca network
  pattern. However, all those bright points that developed into active
  regions emerged at the boundaries of network cells. This suggests that
  the magnetic flux of active regions comes from greater depths in the
  convection zone than the shallow flux that gives rise to the random
  emergence of bright points.

---------------------------------------------------------
Title: Study of the post-flare loops on 29 July 1973. II. Physical
    parameters in the X-ray loops.
Authors: Petrasso, R. D.; Nolte, J. T.; Gerassimenko, M.; Krieger,
   A. S.; Krogstad, R.; Seguin, F. H.; Svestka, Z.
1979SoPh...62..133P    Altcode:
  We use the filter ratio method of analysis to determine spatially
  resolved values of plasma parameters in the X-ray emitting post-flare
  loop system which developed on 29 and 30 July 1973. We find that
  the loops were hotter and had higher plasma pressure at their tops
  than near their footpoints. The loop tops were at nearly the same
  temperature at different places 3 hr after the flare maximum and were
  also at nearly this same temperature 3 and 8 hr later. Variations in
  brightness transverse to the loops were due to variations in emission
  measure. We show by consideration of radiative losses alone that energy
  must have been added to the hottest part of the flare, at the tops of
  the loops, late into the decay phase of the flare.

---------------------------------------------------------
Title: Study of the post-flare loops on 29 July 1973. I. Dynamics
    of the x-ray loops.
Authors: Nolte, J. T.; Gerassimenko, M.; Krieger, A. S.; Petrasso,
   R. D.; Svestka, Z.
1979SoPh...62..123N    Altcode:
  We derive an empirical model of the X-ray emitting post-flare loops
  observed during the decay phase of the 29 July 1973 flare. We find that
  the loops are elliptical, with the brightest emitting region at the
  tops. We determine the height, velocity of growth, and ratio of height
  to width of the loops at times from 3 to 12 hr after the flare onset.

---------------------------------------------------------
Title: Prominences and Solar Activity.
Authors: Svestka, Z.
1979phsp.coll..357S    Altcode: 1979phsp.conf..357S; 1979phsp.coll..356S; 1979IAUCo..44..357S
  Various aspects of solar prominences are discussed. These include
  (1) filament activation, (2) postflare loops, (3) surges and sprays,
  (4) coronal transients, (5) disk vs limb observations, (6) solar
  cycle variations of prominence occurrence, and (7) active prominences
  patrol service.

---------------------------------------------------------
Title: Slowly-Moving Disturbances in the X-Ray Corona.
Authors: Rust, D. M.; Svestka, Z.
1979phsp.coll..276R    Altcode: 1979IAUCo..44..276R; 1979phsp.conf..276R
  A synoptic movie made from nearly 1000 pictures of the solar X-ray
  corona taken by the S-054 X-ray telescope on Skylab has led to
  the discovery of disturbances with propagation velocities under
  100 km/sec and extending over distances of the order of one solar
  radius. The disturbances are revealed as brightened coronal structures
  at progressively greater distances from a central point, usually an
  active region with an activated or disappearing filament. In a number of
  cases these coronal brightenings were accompanied by quiescent filament
  disappearances. The inferred coronal velocities and the rates of damping
  were found to be in excellent agreement with the velocity curves deduced
  by Bruzek (1952), in his slow wave hypothesis, and possibly confirmed
  by Oehman and Oehman (1953) and Yajima (1971) to explain the activation
  of filaments at great distances from flares. The fact that many of
  the events showed little or no flaring associated with the filament
  disappearance at onset leads to the conclusion that the source of the
  slow disturbances is linked to the initial filament eruption itself,
  possibly in restructuring of the magnetic fields or in the coronal
  heating that typically accompanies active region filament eruptions.

---------------------------------------------------------
Title: E. N. Parker first recipient of the George Ellery Hale Prize.
Authors: De Jager, Cornelis; Švestka, Zdeněk
1978SoPh...60....3D    Altcode: 1978SoPh...60....3.
  No abstract at ADS

---------------------------------------------------------
Title: Low-energy protons: Gradients in interplanetary space and
    distribution in the solar corona
Authors: Stevens, G. A.; Vanrooijen, J. J.; Svestka, Z.; De Jager, C.
1978clus.nasa..234S    Altcode:
  First and second order anisotropy measurements are proposed as a tool
  for studying the coronal source function and interplanetary propagation
  of low energy protons. Optimum orbit and attitude requirements are
  suggested for a three telescope system. Some limitations with regard
  to the lower energy limit for a feasible set-up are discussed.

---------------------------------------------------------
Title: Book review
Authors: švestka, Z.
1978SoPh...57..483S    Altcode: 1978SoPh...57..483.
  No abstract at ADS

---------------------------------------------------------
Title: X-Ray Analysis of the 29 July 1973 Flare.
Authors: Nolte, J.; Geras-Simenko, M.; Krieger, A.; Krogstad, R.;
   Petrasso, R.; Seguin, F.; Svestka, Z.
1978BAAS...10Q.457N    Altcode:
  No abstract at ADS

---------------------------------------------------------
Title: Erratum: "Development of a complex of activity in the solar
    corona" [Sol. Phys., Vol. 54, p. 65 - 105 (1977)].
Authors: Howard, R.; Svestka, Z.
1978SoPh...56..471H    Altcode:
  No abstract at ADS

---------------------------------------------------------
Title: Editorial
Authors: De Jager, Cornelis; Švestka, Zdeněk
1978SoPh...56....3D    Altcode: 1978SoPh...56....3.
  No abstract at ADS

---------------------------------------------------------
Title: Do changes in coronal emission structure imply magnetic
    reconnection?
Authors: Nolte, J. T.; Gerassimenko, M.; Krieger, A. S.; Petrasso,
   R. D.; Svestka, Z.; Wentzel, D. G.
1977SoPh...55..401N    Altcode:
  We examine three major possible interpretations of observed
  reconfigurations of coronal X-ray and XUV emitting structures on a scale
  comparable to the size of the structures themselves. One possibility
  is that little change in the large-scale magnetic field configuration
  is associated with the change in emission. The other two possibilities
  are processes by which the magnetic field structure can change.

---------------------------------------------------------
Title: Open magnetic fields in active regions.
Authors: Svestka, Z.; Solodyna, C. V.; Howard, R.; Levine, R. H.
1977SoPh...55..359S    Altcode:
  Soft X-ray observations confirm that some of the dark gaps seen between
  interconnecting loops and inner cores of active regions may be loci of
  open fields, as it has been predicted by global potential extrapolation
  of photospheric magnetic fields. It seems that the field lines may
  open only in a later state of the active region development.

---------------------------------------------------------
Title: Development of a complex of activity in the solar corona.
Authors: Howard, R.; Svestka, Z.
1977SoPh...54...65H    Altcode:
  Skylab observations of the Sun in soft X-rays gave us the first
  possibility to study the development of a complex of activity in the
  solar corona during its whole lifetime of seven solar rotations. The
  basic components of the activity complex were permanently interconnected
  (including across the equator) through sets of magnetic field lines,
  which suggests similar connections also below the photosphere. However,
  the visibility of individual loops in these connections was greatly
  variable and typically shorter than one day. Each brightening of
  a coronal loop in X-rays seems to be related to a variation in the
  photospheric magnetic field near its footpoint. Only loops (rarely
  visible) connecting active regions with remnants of old fields can be
  seen in about the same shape for many days. The interconnecting X-ray
  loops do not connect sunspots.

---------------------------------------------------------
Title: Introductory Talk (Proceedings of the Meeting `How Can Flares
    be Understood?', held during the 16th General Assembly of the IAU
    in Grenoble, France, on 27 August, 1976.)
Authors: Švestka, Zdeněk
1977SoPh...53..221S    Altcode:
  No abstract at ADS

---------------------------------------------------------
Title: Transequatorial loops interconnecting McMath regions 12472
    and 12474.
Authors: Svestka, Z.; Krieger, A. S.; Chase, R. C.; Howard, R.
1977SoPh...52...69S    Altcode:
  We discuss the life-story of a transequatorial loop system which
  interconnected the newly born active region McMath 12474 with the old
  region 12472. The loop system was probably born through reconnection
  accomplished 1.5 to 5 days after the birth of 12474 and the loops were
  observed in soft X-rays for at least 1.5 days. Transient `sharpenings'
  of the interconnection and a striking brightening of the whole loop
  system for about 6 hr appear to be caused by magnetic field variations
  in the region 12474. A flare might have been related to the brightening,
  but only in an indirect way: the same emerging flux could have triggered
  the flare and at the same time strengthened the magnetic field at the
  foot-points of the loops. Electron temperature in the loop system,
  equal to 2.1 × 10<SUP>6</SUP> K in its quiet phase, increased to
  3.1 × 10<SUP>6</SUP> K during the brightening. Electron density in
  the loop system was ≤ 1.3 × 10<SUP>9</SUP> cm<SUP>−3</SUP> and
  it could be estimated to ∼7 × 10<SUP>8</SUP> cm<SUP>−3</SUP>
  prior to the brightening. During the brightening the loops became
  twisted. There was no obvious effect whatsoever of the activity in
  12474 upon the in erconnected old region. The final decay of the loop
  system reflected the decay of magnetic field in the region 12474.

---------------------------------------------------------
Title: Book reviews
Authors: Švestka, Z.
1977SoPh...52..229S    Altcode:
  No abstract at ADS

---------------------------------------------------------
Title: Slowly Moving X-Ray Disturbances from Flares.
Authors: Rust, D. M.; Svestka, Z.
1977BAAS....9..329R    Altcode:
  No abstract at ADS

---------------------------------------------------------
Title: Open Magnetic Fields in Active Regions.
Authors: Svestka, Z.; Solodyna, C. V.; Howard, R.; Levine, R. H.
1977BAAS....9Q.344S    Altcode:
  No abstract at ADS

---------------------------------------------------------
Title: Solar Flares (Book Review)
Authors: Svestka, Z.
1977ApL....18..175S    Altcode:
  No abstract at ADS

---------------------------------------------------------
Title: Low-energy particle events associated with sector boundaries.
Authors: Svestka, Z.; Fritzova-Svestkova, L.; Nolte, J. T.;
   Dodson-Prince, H. W.; Hedeman, E. R.
1976SoPh...50..491S    Altcode:
  Onsets of some 40 to 45 low-energy proton events during the years
  1957-1969 coincided in time with transits of well-defined sector
  boundaries across the Earth. These events can be interpreted as
  long-lived proton streams filling up some of the magnetic sectors,
  indicating an acceleration of protons which is not associated with
  typical proton-producing flares. The sharp onsets of these particle
  streams, as well as a deficiency of flare-associated particle events
  shortly before the boundary transit, indicate that in some cases
  magnetic sector boundaries can inhibit transverse propagation of
  low-energy particles in the solar corona or in interplanetary space.

---------------------------------------------------------
Title: On the occurrence of sympathetic flares.
Authors: Fritzova-Svestkova, L.; Chase, R. C.; Svestka, Z.
1976SoPh...48..275F    Altcode:
  We have tried to determine whether statistical evidence on the
  occurrence of sympathetic flares, which is negative for whole-disk data,
  can be found for particular, physically connected, pairs of active
  regions. Recently, Simnett (1974) and Gergely and Erickson (1975)
  claimed to have found such evidence, but their results were based on
  incorrect computations of the random incidence of flares. If the correct
  formula is applied, the supposed evidence disappears. The results
  are negative also for pairs of active regions interconnected with
  magnetic loops visible in soft X-rays during the Skylab mission. The
  only positive result (with statistical confidence of 3.4 σ) is found
  for pairs of active regions, which are closer than 30° to each
  other, without specifying any kind of physical relationship. For
  such pairs of regions the occurrence of short-time (&lt; 20 min)
  intervals between flares is increased, but the time interval pattern
  does not correspond to any mode of propagation of a triggering agent
  in the solar atmosphere. Therefore, if the increase has real physical
  significance, it would be indicative of some kind of subphotospheric
  synchronization of activity in nearby `sympathetic' active regions.

---------------------------------------------------------
Title: Optical Observations of Flares
Authors: Svestka, Z.
1976RSPTA.281..435S    Altcode: 1976RSLPT.281..435S
  The lecture describes solar flare effects in the chromosphere and
  photosphere, particularly emphasizing problems of the energy transfer,
  and the differences between thermal and non-thermal phases of the
  flare development. Filamentary and shell models are compared and the
  depth of the white-light flare emission is discussed. Optical effects
  possibly associated with other, non-optical flare-associated phenomena
  are pointed out.

---------------------------------------------------------
Title: What should be observed on the sun.
Authors: Svestka, Z.
1976SoPh...47..375S    Altcode:
  Three problems are emphasized in particular: the preflare magnetic
  field configuration, velocity fields, and the nature of acceleration
  processes in flares. It is concluded that what we need most urgently
  are high-resolution hard X-ray, soft X-ray, and EUV-pictures, coronal
  spectra, and magnetograms with high resolution both in space and
  time. A space-shuttle equipped with instrumentation of this kind would
  contribute significantly to our knowledge of the flare process.

---------------------------------------------------------
Title: Low-Energy Particle Events Associated with Sector Boundaries
Authors: Svestka, Z.; Fritzova-Svestkova, L.; Nolte, J. T.;
   Dodson-Prince, H. W.; Hedeman, E. R.
1976BAAS....8R.370S    Altcode:
  No abstract at ADS

---------------------------------------------------------
Title: Flare build-up study
Authors: Svestka, Z.
1976SoPh...47.....S    Altcode: 1976SoPh...47....1S
  The papers deal with problems which might be common to solar flares
  and earth's magnetosphere, problems associated with the initial phases
  of the flare phenomenon, the acceleration processes that seem to occur
  in flares and the magnetosphere, as well as the buildup and storage of
  flare energy in magnetic-field structures. Topics include the active
  role of magnetic fields in providing flare energy, current-sheet models
  of solar flares, the role of plasma turbulence in flare development,
  similarities and differences between magnetospheric substorms and
  solar flares, observations of magnetic merging in earth's magnetotail
  during magnetospheric substorms, evidence for magnetic-energy storage
  in coronal active regions, the possible role of transition-zone
  instabilities in preflare energy buildup, and flare energy storage and
  deposition. Other papers discuss energy release through the interaction
  of coronal magnetic fields, photospheric electric currents as a source
  of flare energy, magnetic-energy buildup in the solar atmosphere,
  magnetic and velocity fields in an active region, flare onset at
  meter wavelengths, laboratory experiments on field-line reconnection,
  key problems in auroral flare processes, and the solar-physics
  Shuttle/Spacelab program. Individual items are announced in this issue.

---------------------------------------------------------
Title: Preface
Authors: de Jager, Cornelis; Obayashi, Tatsuzo; Švestka, Zdeněk
1976SoPh...47....9D    Altcode:
  No abstract at ADS

---------------------------------------------------------
Title: Solar Flares
Authors: Svestka, Z.
1976sofl.book.....S    Altcode: 1976STIN...7634103S
  No abstract at ADS

---------------------------------------------------------
Title: Solar activity (Activité solaire).
Authors: Newkirk, G.; Dunn, R. B.; Mehltretter, P.; MacQueen, R.;
   Bonnet, R. M.; White, O. R.; Fokker, A. D.; Zwaan, C.; Bruzek, A.;
   Durrant, C.; Grossmann-Doerth, U.; Mehltretter, J. P.; Svestka, Z.;
   de Feiter, L. D.; Tandberg-Hanssen, E.; Howard, R.; Stix, M.; Pneuman,
   G. W.; Hundhausen, A. J.; Sawyer, C.; Simon, P.
1976IAUTA..16b..13N    Altcode:
  No abstract at ADS

---------------------------------------------------------
Title: Development of solar active regions.
Authors: Svestka, Z.
1976pspe.proc..129S    Altcode: 1976pspe.conf..129S
  The birth, growth, and decay of solar active regions are described. The
  appearance of active regions in different atmospheric layers is
  examined, and the coronal extension of active regions is considered. The
  use of Skylab soft X-ray and extreme UV observations for studying the
  complex loop structure of active regions in the solar corona and the
  sensitive reactions of the upper atmospheric layers to newly emerging
  flux is explained. It was found that well developed active regions
  are much bigger in the corona than in the underlying sunspot groups
  and plages, and that many of the active regions are connected with
  others through systems of magnetic field lines, occasionally visible in
  soft X-rays. These interconnections, which may survive several solar
  rotations, indicate bigger complexes on the sun than one individual
  active region.

---------------------------------------------------------
Title: Skylab observations of X-ray loops connecting separate
    active regions.
Authors: Chase, R. C.; Krieger, A. S.; Svestka, Z.; Vaiana, G. S.
1976spre.conf..917C    Altcode: 1976spre.proc..917C
  One hundred loops interconnecting 94 separate active solar
  regions detectable in soft X-rays were identified during the Skylab
  mission. While close active regions are commonly interconnected with
  loops, the number of such interconnections decreases steeply for longer
  distances; the longest interconnecting loop observed in the Skylab data
  connected regions separated by 37 deg. Several arguments are presented
  which support the point of view that this is the actual limit of the
  size of magnetic interconnections between active regions. No sympathetic
  flares could be found in the interconnected regions. These results cast
  doubt on the hypothesis that accelerated particles can be guided in
  interconnecting loops from one active region to another over distances
  of 100 deg or more and eventually produce sympathetic flares in them.

---------------------------------------------------------
Title: Solar flares
Authors: Svestka, Z.
1976GAM.....8.....S    Altcode:
  The present book covers all important aspects of solar flares,
  concentrating mainly on flare morphology. Separate chapters
  are devoted to low-temperature flares, high-temperature flares,
  flare-associated optical phenomena, particle emission from flares,
  and flare models. Flare observations in the H-alpha line are discussed
  along with flare spectra, thermal and nonthermal emissions from flares,
  flare waves, and loop prominences. Solar proton and electron emission is
  examined, particle clouds and interplanetary shock waves are considered,
  and characteristics of active regions are reviewed. Flare models are
  described with reference to chromospheric flares, flare synthesis,
  energy sources, energy release and storage, and particle acceleration.

---------------------------------------------------------
Title: Several aspects of flare-associated particle events.
Authors: Svestka, Z.
1976npsa.conf..126S    Altcode:
  No abstract at ADS

---------------------------------------------------------
Title: Book review
Authors: Švestka, Z.
1975SoPh...45..543S    Altcode: 1975SoPh...45..543.
  No abstract at ADS

---------------------------------------------------------
Title: Transequatorial Loops Interconnecting McMath 12472 and 12474.
Authors: Svestka, Z.; Krieger, A.
1975BAAS....7Q.444S    Altcode:
  No abstract at ADS

---------------------------------------------------------
Title: On the behaviour of the hydrogen Lyman series in flares
Authors: de Feiter, L. D.; Svestka, Z.
1975SoPh...41..415D    Altcode:
  The Lyman spectrum of hydrogen has been computed for a number of flare
  models, characterized by the column density of hydrogen atoms in the
  ground state (N<SUB>1</SUB>), the electron density (n<SUB>e</SUB>)
  and the electron temperature (T<SUB>e</SUB>). Broadening by the thermal
  Doppler effect and by Stark effect has been accounted for. The source
  functions for the individual lines of the series have been derived
  from non-LTE calculations of the excitation in hydrogen flares. The
  aim of the investigation is to evaluate the use of the intensities in
  between two successive Lyman lines for a determination of the value
  for N<SUB>1</SUB>, which is a physical parameter of the flare for
  which only indirect determinations are available. Whilst in principle
  this method could give reliable results, its practical application
  meets with difficulties which hardly can be overcome. Therefore, one
  probably has to base the N<SUB>1</SUB> determination on the highest
  line resolvable in the spectrum.

---------------------------------------------------------
Title: Catalog of solar particle events 1955-1969
Authors: Svestka, Z.; Simon, P.
1975ASSL...49.....S    Altcode: 1975cspe.book.....S
  No abstract at ADS

---------------------------------------------------------
Title: On the Acceleration Process in Solar Flares
Authors: Svestka, Z.
1975IAUS...68..427S    Altcode:
  The paper summarizes the data on the acceleration processes on the
  sun. Four different instabilities are distinguished: (1) one with
  purely thermal consequences giving rise to the origin of any flare;
  (2) a nonthermal process at the flash phase of flares giving rise to
  nearby 100 keV electrons and protons, manifested through hard X-ray and
  impulsive microwave bursts; (3) an instability giving rise to streams
  of electrons, without accelerating protons, manifested by type III
  bursts; when (2) and (3) are linked, flare associated electron events in
  space are often recorded; and (4) an explosive instability produces a
  shock wave which manifests itself as a type II burst. This instability
  leads to a second-step acceleration of particles preaccelerated in (2)
  and gives origin to more than 10 MeV protons and relativistic electrons.

---------------------------------------------------------
Title: Catalog of solar particles events, 1955 - 1969.
Authors: Dodson, H. W.; Hedeman, E. R.; Kreplin, R. W.; Martres,
   M. -J.; Obridko, V. N.; Shea, M. A.; Smart, D.; Tanaka, H.; Svestka,
   Z.; Simon, P.; Fritzová-Svestková, L.; Guitart, A.
1975cspe.book.....D    Altcode: 1975QB505.C37......
  No abstract at ADS

---------------------------------------------------------
Title: Type II Radio Bursts and Particle Acceleration
Authors: Švestka, Z.; Fritzová-Švestková, L.
1974SoPh...36..417S    Altcode:
  328 particle events recorded during 30 months from January 1, 1966 to
  June 30, 1968 (taken from the new Catalog of Solar Particle Events,
  1955-1969) are compared with the occurrence of 166 type II radio
  bursts during the same period. The results of this comparison give
  a convincing evidence that proton acceleration to higher energies in
  flares (the `second acceleration step') is closely connected with the
  type II burst occurrence. The shock wave appears to originate near the
  time when the impulsive burst occurs, and the second acceleration step
  follows immediately the first one; in some cases the second step sets
  in while the first step is still in progress.

---------------------------------------------------------
Title: The Hα flare as a secondary product of a coronal instability
Authors: Švestka, Z.
1973SoPh...31..389S    Altcode:
  The assumption that the flare originates in the corona or transition
  layer, is confronted with the known properties of chromospheric
  flares. It is concluded that the basic mode of the energy transport
  into chromosphere is heat conduction. Only in some flares non-thermal
  particles contribute to the brightening in lower atmospheric layers:
  electrons with energy close to 100 keV produce chromospheric
  bright patches, and protons above 20 MeV cause the photospheric
  enhancements. The particle-produced brightenings are superposed on
  the basic quasi-thermal flare and involve only small areas as compared
  with the extensive regions heated through conduction.

---------------------------------------------------------
Title: A Comment on the Flare Activity in August 1972
Authors: Fritzová-Švestková, L.; Švestka}, Z.
1973SoPh...29..417F    Altcode:
  No abstract at ADS

---------------------------------------------------------
Title: Observational Aspects of Flares
Authors: Švestka, Z.
1973str..conf...23S    Altcode:
  No abstract at ADS

---------------------------------------------------------
Title: The Expected Behaviour of the Hydrogen Lyman Lines in Solar
    Flares
Authors: Švestka, Z.; de Feiter, L. D.
1972SSRv...13..824S    Altcode: 1972IAUCo..14..824S
  No abstract at ADS

---------------------------------------------------------
Title: Characteristics of Strong Particle Sources of the Sun
    (Invited Paper)
Authors: Svestka, Z.
1972spen.conf....1S    Altcode:
  No abstract at ADS

---------------------------------------------------------
Title: Editorial
Authors: De Jager, Cornelis; Švestka, Zdeněk
1972SoPh...25....3D    Altcode: 1972SoPh...25....3.
  No abstract at ADS

---------------------------------------------------------
Title: Book review
Authors: Švestka, Z.
1972SoPh...24..498S    Altcode: 1972SoPh...24..498.
  No abstract at ADS

---------------------------------------------------------
Title: Spectral Analysis of Highly Inhomogeneous Chromospheric Flares
Authors: Švestka, Z.
1972SoPh...24..154S    Altcode:
  Analysis of a hydrogen flare spectrum is carried out, assuming
  that the flare radiation is diluted due to a highly inhomogeneous
  space distribution of the flare elements in the chromosphere. It is
  shown that one obtains the correct physical parameters in the flare
  elements, irrespective of the extent of dilution, if all the elements
  are optically thin in the spectral regions considered. However, if
  this is not true for all the elements, the parameters deduced are in
  error, which increases with the extent of dilution. The worst affected
  parameter is the linear thickness of the flaring region which is found
  to be too low by a factor which may be as high as 10. Errors also enter
  into electron and atom densities which are found to be too high and
  into the column density of hydrogen atoms which is underestimated. On
  the other hand, the deduced source function, and in consequence of it
  the electron temperature as well, remain unaffected, if the analysis
  is properly carried out. All the errors may increase strikingly if the
  analysis is performed for optically thick regions. Several kinds of
  observation are mentioned which indicate that dilution of radiation may
  occur in flares. However, reasonable estimates of the flare parameters
  are still possible provided that one avoids spectral regions with τ
  ≳ 1.

---------------------------------------------------------
Title: Spectra of Solar Flares
Authors: Švestka, Zdeněk
1972ARA&A..10....1S    Altcode:
  No abstract at ADS

---------------------------------------------------------
Title: Solar discrete particle events.
Authors: Svestka, Z.
1972sstp.conf...72S    Altcode:
  No abstract at ADS

---------------------------------------------------------
Title: Several Solar Aspects of Flare-Associated Particle Events
Authors: Švestka, Z.
1972PrAA...30..141S    Altcode:
  No abstract at ADS

---------------------------------------------------------
Title: Neutron and gamma-ray emission from white-light flares.
Authors: de Feiter, L. D.; Svestka, Z.
1972spre.conf.1547D    Altcode: 1972spre....2.1547D
  No abstract at ADS

---------------------------------------------------------
Title: Solar Discrete Particle Events
Authors: Švestka, Z.
1972ASSL...29...72S    Altcode: 1972sun..conf...72S
  No abstract at ADS

---------------------------------------------------------
Title: Editorial
Authors: De Jager, Cornelis; Švestka, Zdeněk
1971SoPh...21....3D    Altcode: 1971SoPh...21....3.
  No abstract at ADS

---------------------------------------------------------
Title: On the Flux of Neutrons from Flares
Authors: Švestka, Z.
1971SoPh...19..202S    Altcode:
  Under the assumption that white-light flares are caused by energetic
  particles penetrating into the photosphere (Švestka, 1970a; Najita and
  Orrall, 1970) the known number of protons needed for the white-light
  emission is used to obtain an estimate of the production of neutrons
  occurring at the same time. In the case of the white-light flare of 23
  May, 1967, the peak flux of neutrons at the Earth distance had to exceed
  3 neutrons/cm<SUP>2</SUP>s, thus being detectable in space. This maximum
  neutron flux reached the Earth as early as the time of the maximum
  phase of the flare in the Hα light. However, reasonable estimates
  show that flares associated with a detectable neutron flux should be
  fairly rare phenomena, maybe as rare as the white-light flares.

---------------------------------------------------------
Title: Solar Particle Events
Authors: Svestka, Z.
1971RSPTA.270..157S    Altcode:
  No abstract at ADS

---------------------------------------------------------
Title: Book Review: Intercorrelated satellite observations related
    to solar events. Edited by V. MANNO AND D. E. PAGE. Astrophysics
    and Space Science Library Vol. 19. Springer, New York, and Reidel,
    Dordrecht, Holland, 1970. xvi + 627 pp. Price $38.20
Authors: Švestka, Z.
1971Icar...14..489S    Altcode:
  No abstract at ADS

---------------------------------------------------------
Title: Editorial
Authors: de Jager, Cornelis; Švestka, Zdeněk
1971SoPh...17..287D    Altcode: 1971SoPh...17..287.
  No abstract at ADS

---------------------------------------------------------
Title: Book reviews
Authors: Švestka, Z.; Spiegel, E. A.; van Herk, G.
1971SSRv...11..867S    Altcode:
  No abstract at ADS

---------------------------------------------------------
Title: Solar radio astronomy from the optical solar researchers
    point of view
Authors: Svestka, Z.
1971cesra...1...15S    Altcode:
  No abstract at ADS

---------------------------------------------------------
Title: The Phase of Particle Acceleration in the Flare Development
Authors: Švestka, Z.
1970SoPh...13..471S    Altcode:
  Evidence is given that the particle acceleration in flares is confined
  to the initial phase of the flare development preceding the Hα flare
  maximum and lasting for less than 10 min. The impulsive acceleration
  process is confined to a relatively small limited volume of about 5
  × 10<SUP>27</SUP> cm<SUP>3</SUP> in the region of highest magnetic
  gradient in the flare, and its size represents about 0.05 or less of
  the total extent of the hot condensation which produces the soft X-ray
  and gradual microwave bursts. About one in fifty particles in this
  volume is accelerated to energy exceeding 100 keV, the total particle
  density being ≈ 10<SUP>10</SUP> cm<SUP>−3</SUP>. The accelerated
  electrons produce the impulsive hard X-ray burst, but synchrotron losses
  greatly reduce the number of relativistic electrons participating in
  the bremsstrahlung process. Protons above 20 MeV penetrate to the
  lowest chromosphere and upper photosphere and temporarily increase
  the temperature in the bombarded region. As the result a flash of
  continuous emission appears, which should be most expressive below
  1527 Å. The associated white-light emission shows the bottom of the
  region where the impulsive acceleration process occurs.

---------------------------------------------------------
Title: Book Review: Astronomy and Astrophysics Abstracts, Vol. 1:
    Literature 1969, Part 1, Springer-Verlag, Berlin, Heidelberg, New York
Authors: Švestka, Z.
1970SoPh...12R.502S    Altcode: 1970SoPh...12R.502Z
  No abstract at ADS

---------------------------------------------------------
Title: Solar Activity.
Authors: Svestka, Z.
1970IAUTA..14...71S    Altcode:
  No abstract at ADS

---------------------------------------------------------
Title: Solar particle events.
Authors: Svestka, Z.
1970spre.conf..797S    Altcode:
  No abstract at ADS

---------------------------------------------------------
Title: Book Review: Annals of the IQSY, M. I. T. Press, Vols. 1-5
Authors: Švestka, Z.
1970SoPh...12Q.502S    Altcode: 1970SoPh...12Q.502Z
  No abstract at ADS

---------------------------------------------------------
Title: Particle Event Forecasting
Authors: Švestka, Z.
1970ASSL...19...90S    Altcode: 1970iso..conf...90S
  No abstract at ADS

---------------------------------------------------------
Title: The solar proton flares of June and November 1968 and
    February 1969.
Authors: Krivský, L.; Svestka, Z.
1970spre.conf..817K    Altcode:
  No abstract at ADS

---------------------------------------------------------
Title: Editorial
Authors: De Jager, Cornelis; Švestka, Zdeněk
1969SoPh...10..243D    Altcode: 1969SoPh...10..243.
  No abstract at ADS

---------------------------------------------------------
Title: Proton Flare Project, 1966. Summary of the August/September
    Particle Events in the McMath Region 8461. (Invited Review Paper)
Authors: Švestka, Z.; Simon, P.
1969SoPh...10....3S    Altcode:
  The paper summarizes observations of solar and space phenomena related
  to the McMath region Number 8461 which passed over the solar disk during
  the 1966 Proton Flare Project period, from August 21 to September 4,
  and produced two important solar particle events on August 28 and
  September 2. The most important results are reviewed and interpretation
  of some of them is suggested.

---------------------------------------------------------
Title: Comment on the Note by Friedman and Hamberger
Authors: Švestka, Z.
1969SoPh....8..400S    Altcode:
  No abstract at ADS

---------------------------------------------------------
Title: Editorial
Authors: Švestka, Z.; De Jager, C.
1969SoPh....8....3S    Altcode: 1969SoPh....8....3.
  No abstract at ADS

---------------------------------------------------------
Title: Abstracts of papers from other journals
Authors: Pasachoff, Jay M.; Gussmann, E. A.; Stepanyan, N. N.; de
   Feiter, L. D.; Uchida, Yutaka; Švestka, Z.; Vassilyeva, G. J.
1969SoPh....6..155P    Altcode:
  No abstract at ADS

---------------------------------------------------------
Title: The optical flare
Authors: Švestka, Z.
1969sfsr.conf...16S    Altcode:
  No abstract at ADS

---------------------------------------------------------
Title: Solar flares and space research
Authors: de Jager, C.; Svestka, Z.
1969sfsr.conf.....D    Altcode: 1969sfsr.book.....D
  No abstract at ADS

---------------------------------------------------------
Title: Effects associated with the sector boundary crossing on 8
    July 1966
Authors: Švestka, Z.
1969sfsr.conf..319S    Altcode:
  No abstract at ADS

---------------------------------------------------------
Title: General summary on the results of the first Proton Flare
    Project period, July 1966.
Authors: Simon, P.; Svestka, Z.
1969AIQSY...3..469S    Altcode:
  No abstract at ADS

---------------------------------------------------------
Title: Editorial
Authors: De Jager, C.; Švestka, Z.
1968SoPh....5..259D    Altcode: 1968SoPh....5..259.
  No abstract at ADS

---------------------------------------------------------
Title: Effects associated with the Sector Boundary crossing on July
    8, 1966
Authors: Švestka, Zdeněk.
1968SoPh....4..361S    Altcode:
  Thirty hours after the proton flare of July 7, 1966, the earth and
  nearby satellites crossed a sector boundary of the interplanetary
  magnetic field. This occurred before the flare-associated shockwave
  arrived at the earth, so that the space was filled with energetic
  particles ejected from the flare. Satellite measurements have shown
  that in such a case &lt;20 MeV protons are stored within the range of
  the sector boundary and with decreasing energy the particles tend to
  accumulate towards and behind the Eastern boundary limit; low-energy
  particles, such as &lt;50 keV electrons, are stored exclusively behind
  this Eastern limit.

---------------------------------------------------------
Title: On Long-Term Forecasts of Proton Flares
Authors: Švestka, Zdeněk.
1968SoPh....4...18S    Altcode:
  174 proton flares which were observed during the period from 1956 to
  1965, occurred in 81 different active regions. It is shown that these
  active regions formed in complexes of activity, which stayed on the
  solar surface for many months, and in some cases even for several
  years. Since the proton-flare regions develop very rapidly and reach
  the proton-flare active stage within a few days, these complexes of
  activity represent the areas on the sun, where proton-flare regions
  can form at any time. Reference is made to contributions by Bumba and
  Howard, who investigated the birth of active regions and detected some
  properties of complexes of activity; nevertheless, at the present time,
  we do not know any method to predict when a proton-flare region begins
  to develop in such a complex of activity.

---------------------------------------------------------
Title: Introduction and Summary
Authors: Svestka, Z.
1968IAUS...35..513S    Altcode:
  No abstract at ADS

---------------------------------------------------------
Title: Mass motions in flares indicated by line profiles and
    filtergrams Introductory lecture
Authors: Švestka, Z.
1968mmsf.conf...17S    Altcode:
  No abstract at ADS

---------------------------------------------------------
Title: Loop-Prominence Systems and Proton-Flare Active Regions
Authors: Svestka, Z.
1968IAUS...35..287S    Altcode:
  No abstract at ADS

---------------------------------------------------------
Title: Editorial
Authors: De Jager, C.; Švestka, Z.
1968SoPh....3....3D    Altcode: 1968SoPh....3....3.
  No abstract at ADS

---------------------------------------------------------
Title: Electron Density in Flares, II: Results of Measurement
Authors: Fritzová-Švestková, L.; Švestka, Z.
1967SoPh....2...87F    Altcode:
  Measurements of the electron density in 16 flares are summarized and
  discussed. For 13 of them the electron density has been determined by
  the halfwidth method discussed in Part I of this paper. In the flash
  phase of all disk flares of importance 1 + and higher the electron
  density exceeds 10<SUP>13</SUP> cm<SUP>−3</SUP> and increases with
  the flare importance. In the maximum of large flares the electron
  density exceeds 3 × 10<SUP>13</SUP> cm<SUP>−3</SUP> and declines
  to 10<SUP>13</SUP> cm<SUP>−3</SUP> and to lower values in about
  20 minutes after the flash phase. In limb flares, i.e. higher than
  5000 km above the solar limb, the electron density is lower than 5
  × 10<SUP>12</SUP> cm<SUP>−3</SUP>. This shows a decrease of the
  electron density in the flare elements situated in higher parts of the
  chromosphere. On the other hand, however, at least in some flares the
  electron density remains fairly constant within a wide range of height
  in the upper chromosphere and the low corona.

---------------------------------------------------------
Title: Electron Density in Flares, I: Discussion of the Halfwidth
    Method
Authors: Švestka, Z.; Fritzová-Švestková, L.
1967SoPh....2...75S    Altcode:
  The halfwidth method used for the determination of the electron
  density in flares is discussed from the point of view of possible
  errors which may enter the obtained results. The discussion includes
  an analysis of errors of measurement as well as errors of the method
  due to: (1) our incomplete knowledge of the electron damping, (2)
  the assumption of constant electron temperature, (3) the presence
  of residual self-absorption in high Balmer lines, and (4) possibly
  present non-thermal motions. It is shown that the factors (2) to (4)
  cannot induce any relative error in n<SUB>e</SUB> higher than 30 %
  of the correct value, and the actual error usually is smaller. A
  comparison is made of the halfwidth-method application to active
  prominences and limb flares.

---------------------------------------------------------
Title: Editorial
Authors: de Jager, C.; Švestka, Z.
1967SoPh....1..303D    Altcode: 1967SoPh....1..303.
  No abstract at ADS

---------------------------------------------------------
Title: Type IV bursts. III. In association with Forbush effects
Authors: Švestka, Z.
1967BAICz..18...55S    Altcode:
  No abstract at ADS

---------------------------------------------------------
Title: Editorial
Authors: de Jager, C.; Švestka, Z.
1967SoPh....1....3D    Altcode: 1967SoPh....1....3.
  No abstract at ADS

---------------------------------------------------------
Title: Buchbesprechungen über: Solar Physics. Ed. C. DE JAGER,
    and Z. ŠVESTKA. (Ref. R. O. REDMAN)
Authors: de Jager, C.; Švestka, Z.
1967ZA.....67...95D    Altcode:
  No abstract at ADS

---------------------------------------------------------
Title: Optical Observations of Solar Flares
Authors: Švestka, Zdeněk
1966SSRv....5..388S    Altcode:
  This paper gives a review of the results of optical observations of
  solar flares. Observations carried out in the H<SUB>α</SUB> line,
  flare spectra, and the methods of analysing the flare spectra are
  briefly discussed. Great attention is paid to the continuous emission
  of flares in the optical spectral region. In the last section, optical
  aspects of proton flares are summarized.

---------------------------------------------------------
Title: Type IV bursts. II. In association with PCA events
Authors: Fritzová-Švestková, L.; Švestka, Z.
1966BAICz..17..249F    Altcode:
  No abstract at ADS

---------------------------------------------------------
Title: The H- emission in flares
Authors: Švestka, Z.
1966BAICz..17..137S    Altcode:
  No abstract at ADS

---------------------------------------------------------
Title: Proton flares before 1956
Authors: Švestka, Z.
1966BAICz..17..262S    Altcode:
  No abstract at ADS

---------------------------------------------------------
Title: A prediction on proton flare occurrence in 1966-1968
Authors: Švestka, Z.
1966BAICz..17...95S    Altcode:
  No abstract at ADS

---------------------------------------------------------
Title: Type IV Bursts. I. List of events
Authors: Švestka, Z.; Olmr, J.
1966BAICz..17....4S    Altcode:
  No abstract at ADS

---------------------------------------------------------
Title: Spectral Analysis of Solar Flares
Authors: Švestka, Zdeněk
1965AdA&A...3..119S    Altcode:
  No abstract at ADS

---------------------------------------------------------
Title: Spectral anomalies associated with the extraordinary X-ray
    emission recorded by the SR-1 satellite on August 7, 1960
Authors: Svestka, Z.
1964spre.conf..768S    Altcode:
  No abstract at ADS

---------------------------------------------------------
Title: Electron temperature and b<SUB>n</SUB> values in flares
Authors: Švestka, Z.
1964BAICz..15...38S    Altcode:
  No abstract at ADS

---------------------------------------------------------
Title: Broadening of high Balmer lines in flares and prominences
Authors: Švestka, Z.
1964BAICz..15..162S    Altcode:
  No abstract at ADS

---------------------------------------------------------
Title: Time variation of electron density in a large solar flare
Authors: de Feiter, L. D.; Švestka, Z.
1964BAICz..15..117D    Altcode:
  No abstract at ADS

---------------------------------------------------------
Title: Qualitative discussion of 244 flare spectra. IV. Splitting
    of metal emission lines
Authors: Kopecký, M.; Letfus, V.; Blaha, M.; Švestka, Z.
1963BAICz..14..146K    Altcode:
  No abstract at ADS

---------------------------------------------------------
Title: On the spectral analysis of flares
Authors: Švestka, Z.
1963BAICz..14...75S    Altcode:
  No abstract at ADS

---------------------------------------------------------
Title: Spectral analysis of the moustache-like flare of August 7, 1960
Authors: Svestka, Z.
1963BAICz..14..234S    Altcode:
  No abstract at ADS

---------------------------------------------------------
Title: Astronomicky a astronauticky slovnik.
Authors: Kleczek, Josip; Svestka, Zdenek
1963aaas.book.....K    Altcode: 1963QB14.K56.......
  No abstract at ADS

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Title: Evidence of Stark broadening of Balmer lines in flares
Authors: Svestka, Z.
1962BAICz..13..236S    Altcode:
  No abstract at ADS

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Title: Qualitative discussion of 244 flare spectra. II. Line asymmetry
    and helium lines
Authors: Švestka, Z.; Kopecký, M.; Blaha, M.
1962BAICz..13...37S    Altcode:
  No abstract at ADS

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Title: Motions in chromospheric flares
Authors: Švestka, Z.
1962BAICz..13..190S    Altcode:
  No abstract at ADS

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Title: Note on planetary nebulae in the Small Magellanic Cloud
Authors: Švestka, Z.
1962BAICz..13...35S    Altcode:
  No abstract at ADS

---------------------------------------------------------
Title: On a peculiar flare spectrum
Authors: Švestka, Z.
1962BAICz..13...30S    Altcode:
  No abstract at ADS

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Title: Qualitative discussion of 244 flare spectra. III. Metal
    emission lines
Authors: Blaha, M.; Kopecký, M.; Švestka, Z.
1962BAICz..13...85B    Altcode:
  No abstract at ADS

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Title: Qualitative discussion of 244 flare spectra
Authors: Švestka, Z.; Kopecký, M.; Blaha, M.
1961BAICz..12..229S    Altcode:
  No abstract at ADS

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Title: Observations of flares at the Ondřejov Observatory in the
    year 1959
Authors: Kvičala, F.; Hřebik, F.; Olmr, F.; Švestka, Z.;
   Křivský, L.
1961BAICz..12...47K    Altcode:
  No abstract at ADS

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Title: Spectrum of the flare of July 20, 1958
Authors: Švestka, Z.
1961BAICz..12...73S    Altcode:
  No abstract at ADS

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Title: Measurement of Magnetic Fields in Chromospheric Flares
Authors: Blaha, M.; Kopecký, M.; Švestka, Z.
1960Natur.187..224B    Altcode:
  SPECTRA of two great chromospheric flares taken by the flare
  spectrograph at Ondřejov<SUP>1</SUP> show an evident splitting of the
  D<SUP>1</SUP> emission line of Na I which is attributed to a magnetic
  field existing in that part of the chromosphere where the sodium lines
  are formed. This explanation is supported by the following facts :

---------------------------------------------------------
Title: List of flares observed at Ondrejov observatory during
    the I.G.Y.
Authors: Kvicala, J.; Hrebik, F.; Letfus, V.; Olmr, J.; Svestka, Z.;
   Krivsky, L.
1960PAICz..43....1K    Altcode:
  No abstract at ADS

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Title: Hydrogen spectrum of the flare of July 30, 1959
Authors: Švestka, Z.
1960BAICz..11..167S    Altcode:
  No abstract at ADS

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Title: The flare spectrograph at Ondřejov
Authors: Valníček, B.; Letfus, V.; Blaha, M.; Švestka, Z.; Seidl, Z.
1959BAICz..10..149V    Altcode:
  No abstract at ADS

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Title: Catalogue of Chromospheric Flares observed at Ondřejov during
    the first half of the year 1957
Authors: Letfus, V.; Růžičková, B.; Švestka, Z.
1959BAICz..10..136L    Altcode:
  No abstract at ADS

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Title: Damping and Stark broadening of Balmer lines
Authors: Švestka, Z.
1959BAICz..10...10S    Altcode:
  No abstract at ADS

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Title: Polarization of Light of the Comets Arend-Roland (1956h)
    and Mrkos (1957d)
Authors: Blaha, M.; Hruška, A.; Švestka, Z.; Vanýsek, V.
1958Natur.182..331B    Altcode:
  POLARIZATION of the total light of the Comets 1956h and 1957d
  was studied photographically by simultaneous exposures with three
  objectives and three `Polaroids'. The planes of polarization of the
  three `Polaroids' were at 120°. 2-in. objectives were used at ƒ/9
  with Agfa `Astro' panchromatic plates. The characteristic curve was
  determined by comparison with an exposed photometric wedge. Errors due
  to the instrument were measured by means of light from an artificial
  source, polarized to a known degree by reflexion from a glass
  surface. The error of the polarization determined is +/- 2.5 per cent.

---------------------------------------------------------
Title: Catalogue of chromospheric flares observed at Ondřejov during
    the years 1952-1956
Authors: Letƒus, V.; RůžiČková, B.; Švestka, Z.
1958BAICz...9..178L    Altcode:
  No abstract at ADS

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Title: 536 Mc/s radio events associated with chromospheric flares
    during the year 1956
Authors: Budějický, J.; Švestka, Z.
1958BAICz...9...48B    Altcode:
  No abstract at ADS

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Title: Fysikalni podminky V chromosferickych erupcich.
Authors: Svestka, Zdenek
1957PAICz..32.....S    Altcode: 1957QB1.C284A3c32..
  No abstract at ADS

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Title: Mezihvezdna hmota.
Authors: Svestka, Zdenek; Vanysek, Valdimir
1956mehm.book.....S    Altcode: 1956QB500.S9.......
  No abstract at ADS

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Title: Several Notes on the Statistics of Chromosferic Flares
Authors: Švestka, Z.
1956BAICz...7....9S    Altcode:
  No abstract at ADS

---------------------------------------------------------
Title: The Optical Thickness of Flares and the Broadening of Balmer
    Lines in their Spectra
Authors: Švestka, Z.
1956BAICz...7..130S    Altcode:
  No abstract at ADS

---------------------------------------------------------
Title: The Width of H<SUB>α</SUB> in Solar Flares
Authors: Švestka, Z.; Fritzová, L.
1956BAICz...7...30S    Altcode:
  No abstract at ADS

---------------------------------------------------------
Title: Secondary Periods of Long-periodic Variables
Authors: Fritzová, L.; Pěkný, Z.; Švestka, Z.
1954BAICz...5...49F    Altcode:
  No abstract at ADS

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Title: Hvezdne atmosfery.
Authors: Svestka, Zdenek
1954hvat.book.....S    Altcode: 1954QB809.S85......
  No abstract at ADS

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Title: Catalogue des crateres lunaire
Authors: Bouska, J.; Hrebik, F.; Svestka, Z.
1953PAICz..25..107B    Altcode:
  No abstract at ADS

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Title: Recurrent and Revived Active Regions on the Sun
Authors: Švestka, Z.
1953BAICz...4..186S    Altcode:
  No abstract at ADS

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Title: Slunce a jeho vlivy NA zemi.
Authors: Link, Frantisek; Svestka, Zdenek
1953sajv.book.....L    Altcode: 1953QB521.L72......
  No abstract at ADS

---------------------------------------------------------
Title: The H<SUB>α</SUB>-Emission from Chromospheric Flares:
    Central Intensity and Line-Width
Authors: Švestka, Z.
1951BAICz...2..165S    Altcode:
  No abstract at ADS

---------------------------------------------------------
Title: The H<SUB>α</SUB>-Emission from Chromospheric Flares: The
    Flare of August 5, 1949
Authors: Švestka, Z.
1951BAICz...2..153S    Altcode:
  No abstract at ADS

---------------------------------------------------------
Title: The H<SUB>α</SUB>-Emission from Chromospheric Flares:
    Expanding Source of Radiation
Authors: Švestka, Z.
1951BAICz...2..150S    Altcode:
  No abstract at ADS

---------------------------------------------------------
Title: The H<SUB>α</SUB>-Emission from Chromospheric Flares: Course
    of the Asymmetry
Authors: Švestka, Z.
1951BAICz...2..120S    Altcode:
  No abstract at ADS

---------------------------------------------------------
Title: The H<SUB>α</SUB>-Emission from Chromospheric Flares:
    General Features of the Asymmetry
Authors: Švestka, Z.
1951BAICz...2..100S    Altcode:
  No abstract at ADS

---------------------------------------------------------
Title: The H<SUB>α</SUB>-Emission from Chromospheric Flares:
    Observations
Authors: Švestka, Z.
1951BAICz...2...81S    Altcode:
  No abstract at ADS

---------------------------------------------------------
Title: On a Possible Development of Planetary Nebulae
Authors: Švestka, Z.
1950BAICz...2...52S    Altcode:
  No abstract at ADS

---------------------------------------------------------
Title: The Reason of Validity of the Bode's Law
Authors: Švestka, Z.
1950BAICz...2...45S    Altcode:
  No abstract at ADS

---------------------------------------------------------
Title: A Note on the Brightness of Lunar Eclipses
Authors: Švestka, Z.
1950BAICz...2...41S    Altcode:
  No abstract at ADS

---------------------------------------------------------
Title: On the Variations of the Enlargement of the Earth's Shadow
    during the Lunar Eclipses
Authors: Švestka, Z.
1950BAICz...2....6S    Altcode:
  No abstract at ADS

---------------------------------------------------------
Title: The Influence of Clouds on the Density of the Central Part
    of the Earth's Shadow
Authors: Švestka, Zdeněk.
1949BAICz...1..131S    Altcode:
  No abstract at ADS

---------------------------------------------------------
Title: On the Variation of the Coma-Diameter of Encke's Comet
Authors: Bouška, Jiří.; Švestka, Zdeněk.
1949BAICz...1..123B    Altcode:
  No abstract at ADS

---------------------------------------------------------
Title: On the Observed Density of the Earth's Shadow near its Centre
Authors: Švestka, Zdeněk.
1949BAICz...1..109S    Altcode:
  No abstract at ADS

---------------------------------------------------------
Title: On the Real Number of Solar Flares
Authors: Švestka, Zdeněk.
1949BAICz...1...95S    Altcode:
  No abstract at ADS

---------------------------------------------------------
Title: Observations of Solar Flares and High-speed Prominences from
    July to December 1948
Authors: Švestka, Zdeněk.
1949BAICz...1...73S    Altcode:
  No abstract at ADS

---------------------------------------------------------
Title: The Illumination by Diffusion in the Centre of the Earth's
    Shadow
Authors: Švestka, Zdeněk.
1948BAICz...1...48S    Altcode:
  No abstract at ADS

---------------------------------------------------------
Title: The Density of the Earth's Shadow near its Centre
Authors: Švestka, Zdeněk.
1948BAICz...1...29S    Altcode:
  No abstract at ADS