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Author name code: kashapova
ADS astronomy entries on 2022-09-14
author:"Kashapova, Larisa K." 

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Title: Analysis of the Properties of SEP Events and Their
    Solar Sources Taking Into Account of the Magneto-Morphological
    Classification of Active Regions
Authors: Kashapova, L. K.; Zhukova, A. V.; Miteva, R.; Zhdanov, D. A.;
   Myagkova, I. N.; Meshalkina, N. S.
2021Ge&Ae..61.1022K    Altcode:
  We studied 87 events of solar cosmic rays, i.e., solar energetic
  particle (SEP) emissions associated with solar flares of at least
  M5 class (according to the GOES classification) that occurred during
  solar cycle 23. A relationship between the spectral parameters of the
  SEP events and the microwave (MW) emission properties of the related
  solar flares was analysed. The peak frequency of the MW spectrum
  was used as an indicator of the acceleration processes during solar
  flares, which may characterize both the strength of magnetic field
  in the emission source and the intensity of the accelerated particle
  flux. The magneto-morphological classification (MMC) was applied to
  take into account the features of the magnetic topology of the active
  regions (ARs) that generated flares. Our analysis showed that most
  of ARs, associated with SEP events with large proton flux, violated
  at least one of the empirical laws established for sunspot groups
  (Hale's law, Joy's law, or another). The relationships between the
  spectral properties of electrons and protons and the properties of MW
  radiation were analyzed and discussed, taking into account the MMC of
  ARs generated flares associated with SEP events.

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Title: Common Origin of Quasi-Periodic Pulsations in Microwave and
    Decimetric Solar Radio Bursts
Authors: Kashapova, Larisa K.; Kolotkov, Dmitrii Y.; Kupriyanova, Elena
   G.; Kudriavtseva, Anastasiia V.; Tan, Chengming; Reid, Hamish A. S.
2021SoPh..296..185K    Altcode: 2021arXiv211007880K
  We analyse quasi-periodic pulsations (QPP) detected in the
  microwave and decimetre radio emission of the 5 May 2017 7:04 UT
  (SOL2017-09-05T07:04) solar flare, using simultaneous observations
  by the Siberian Radioheliograph 48 (SRH-48, 4 - 8 GHz) and Mingantu
  Spectral Radioheliograph (MUSER-I, 0.4 - 2 GHz). The microwave
  emission was broadband with a typical gyrosynchrotron spectrum, while
  a quasi-periodic enhancement of the decimetric emission appeared
  in a narrow spectral band (500 - 700 MHz), consistent with the
  coherent-plasma-emission mechanism. The periodicity that we found
  in microwaves is about 30 seconds, coming from a compact loop-like
  source with a typical height of about 31 Mm. The decimetric emission
  exhibited a periodicity of about 6 seconds. We suggest a qualitative
  scenario linking the QPPs observed in both incoherent and coherent
  spectral bands and their generation mechanisms. The properties of the
  QPPs found in the microwave signal are typical for perturbations of the
  flare loop by the standing sausage mode of a fast magnetohydrodynamic
  (MHD) wave. Our analysis indicated that this sausage-oscillating
  flare loop was the primary source of oscillations in the discussed
  event. The suggested scenario is that a fundamental sausage harmonic is
  the dominant cause for the observed QPPs in the microwave emission. The
  initiation of oscillations in the decimetric emission is caused by the
  third sausage harmonic via periodic and nonlinear triggering of the
  acceleration processes in the current sheets, formed at the interface
  between the sausage-oscillating flare loop and the external coronal loop
  that extended to higher altitudes. Our results demonstrate the possible
  role of MHD wave processes in the release and transport of energy during
  solar flares, linking coherent and incoherent radio emission mechanisms.

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Title: Analysis of the Eruptive Event after the Solar Flare of June
    7, 2011
Authors: Kupryakov, Yu. A.; Gorshkov, A. B.; Kotrč, P.; Kashapova,
   L. K.
2021ARep...65..876K    Altcode:
  We present the results of the analysis of the observational data
  for the eruptive event of June 7, 2011 obtained both on spacecraft
  (SDO, LASCO) and using ground-based solar instruments. The event was
  characterized by deceleration of the shock front during the first
  minutes of the evolution from 1150 to 710 km/s. According to the
  LASCO data, the velocity of the coronal mass ejection (CME) on time
  scales of more than an hour did not exceed 285 km/s. According to the
  spectral observations of the ground-based instrument, we found the
  radial velocities of the fastest features of the exploding prominence
  to be between 200 and 190 km/s. We paid special attention to studying
  the physical characteristics of a blob—a separate drop of coronal
  rain that accompanied the event. The line-of-sight velocity of the
  blob increased in 5 min from 207 to 263 km/s, its diameter was 5900
  km, and the estimated mass was 1.8 × 10<SUP>12</SUP> g; the values
  of temperature and turbulent velocity of 7880 K and V<SUB>turb</SUB>
  = 18.7 km/s were obtained,correspondingly. We should note that the
  finding and measurement of velocities were limited by the capabilities
  of narrow-band filters and a small wavelength range in most solar
  instruments. This paper is based on the report made at the conference
  "Ideas of S.B. Pikelner and S.A. Kaplan and Modern Astrophysics"
  (Sternberg Astronomical Institute, Moscow State University, February
  8-12, 2021).

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Title: The morphology of average solar flare time profiles from
    observations of the Sun's lower atmosphere
Authors: Kashapova, Larisa K.; Broomhall, Anne-Marie; Larionova,
   Alena I.; Kupriyanova, Elena G.; Motyk, Ilya D.
2021MNRAS.502.3922K    Altcode: 2021MNRAS.tmp..301K; 2021arXiv210202596K
  We study the decay phase of solar flares in several spectral bands
  using a method based on that successfully applied to white light flares
  observed on an M4 dwarf. We selected and processed 102 events detected
  in the Sun-as-a-star flux obtained with SDO/AIA images in the 1600 and
  304 Å channels and 54 events detected in the 1700 Å channel. The main
  criterion for the selection of time profiles was a slow, continuous
  flux decay without significant new bursts. The obtained averaged time
  profiles were fitted with analytical templates, using different time
  intervals, that consisted of a combination of two independent exponents
  or a broken power law. The average flare profile observed in the 1700
  Å channel decayed more slowly than the average flare profile observed
  on the M4 dwarf. As the 1700 Å emission is associated with a similar
  temperature to that usually ascribed to M dwarf flares, this implies
  that the M dwarf flare emission comes from a more dense layer than
  solar flare emission in the 1700 Å band. The cooling processes in solar
  flares were best described by the two exponents model, fitted over the
  intervals t1 = [0, 0.5]t<SUB>1/2</SUB> and t2 = [3, 10]t<SUB>1/2</SUB>,
  where t<SUB>1/2</SUB> is time taken for the profile to decay to half
  the maximum value. The broken power-law model provided a good fit to
  the first decay phase, as it was able to account for the impact of
  chromospheric plasma evaporation, but it did not successfully fit the
  second decay phase.

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Title: Analysis of Properties of SEP Events and their Solar Sources
    Considering the Magneto- Morphology Classification of Active Regions
Authors: Zhukova, A. V.; Kashapova, L. K.; Miteva, R.; Zhdanov, D. A.;
   Meshalkina, N. S.; Myagkova, I. N.
2020acsp.conf..105Z    Altcode:
  No abstract at ADS

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Title: The origin of quasi-periodicities during circular ribbon flares
Authors: Kashapova, L. K.; Kupriyanova, E. G.; Xu, Z.; Reid, H. A. S.;
   Kolotkov, D. Y.
2020A&A...642A.195K    Altcode: 2020arXiv200802010K
  Context. Solar flares with a fan-spine magnetic topology are able to
  form circular ribbons. A previous study based on Hα line observations
  of the solar flares on 5 March 2014 revealed a uniform and continuous
  rotation of the magnetic fan-spine. A preliminary analysis of the flare
  time profiles revealed quasi-periodic pulsations (QPPs) with similar
  properties in hard X-rays, Hα, and microwaves. <BR /> Aims: In this
  work, we address the question of whether the observed periodicities are
  related to periodic acceleration of electrons or plasma heating. <BR />
  Methods: We analysed QPPs in the Hα emission from the centre of the
  fan (inner ribbon R1), a circular ribbon (R2), a remote source (R3),
  and an elongated ribbon (R4) located between R2 and R3. We used methods
  of correlation, Fourier, wavelet, and empirical mode decomposition. We
  compared the QPPs in Hα emission with those in microwave and X-ray
  emission. <BR /> Results: We found multi-wavelength QPPs with periods
  around 150 s, 125 s, and 190 s. The 150 s period is seen to co-exist
  in Hα, hard X-rays, and microwave emissions, which allowed us to
  connect it with flare kernels R1 and R2. These kernels spatially
  coincide with the site of the primary flare energy release. The 125
  s period is found in the Hα emission of the elongated ribbon R4 and
  the microwave emission at 5.7 GHz during the decay phase. The 190
  s period is present in the emission during all flare phases in the
  Hα emission of both the remote source, R3, and the elongated ribbon,
  R4, in soft X-rays and in microwaves at 4-8 GHz. <BR /> Conclusions:
  We connected the dominant 150 s QPPs with the slipping reconnection
  mechanism occurring in the fan. We suggested that the period of 125
  s in the elongated ribbon can be caused by a kink oscillation of the
  outer spine, connecting the primary reconnection site with the remote
  footpoint. The period of 190 s is associated with the three-minute
  sunspot oscillations.

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Title: Calculation of the intensity of Mg I spectral lines in solar
    prominences using the Cloudy code model
Authors: Kupryakov, Yu. A.; Dodin, A. V.; Schwartz, P.; Kashapova,
   L. K.
2020A&AT...31..459K    Altcode:
  Spectroscopical observations of several prominences in the MgI lines
  were carried out from 2014 to 2017. These lines from visible part of
  the solar spectrum play an important diagnostic role, complementing the
  UV Mg II resonance lines regularly observed by the IRIS satellite. We
  found that a rather weak Mg I emission, e.g., in the 5172.6 Å line
  correlates well with the presence of extended bright areas on the solar
  disk observed in the 1600 Å SDO / AIA band. However, in many cases
  the radiation in the 5172.6 Å line is very low, even not detectable,
  although a bright prominence above the limb or are <P />on the solar
  disc were observed. To explain this phenomenon, we have calculated
  spectra of optically thin plasma using Cloudy code and found that
  observed ratio of optical lines and UV continuum is possible and the
  presence of heel processes stimulates luminescence in Mg I and 1600
  Å lines.

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Title: The Calculation of the Intensity of The Mg I Spectral Lines
    in Solar Prominences Using the Cloudy code Model
Authors: Kupryakov, Yu. A.; Dodin, A. V.; Schwartz, P.; Kashapova,
   L. K.
2019simi.conf..139K    Altcode: 2019simi.conf..139D
  Spectroscopical observations of several prominences in the MgI lines
  were carried out from 2014 to 2017. These lines from visible part of
  the solar spectrum play an important diagnostic role, complementing the
  UV Mg II resonance lines regularly observed by the IRIS satellite. We
  found that a rather weak Mg I emission, e.g., in the 5172.6 Å line
  correlates well with the presence of extended bright areas on the
  solar disk observed in the 1600 Å SDO/AIA band. However, in many cases
  the radiation in the 5172.6 Å line is very low, even not detectable,
  although a bright prominence above the limb or flare on the solar disc
  were observed. To explain this phenomenon, we have calculated spectra
  of optically thin plasma using Cloudy code and found that observed
  ratio of optical lines and UV continuum is possible and the presence
  of heel processes stimulates luminescence in Mg I and 1600 Å lines.

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Title: Features of Solar Energetic Particle Events During the 23rd
    Cycle Of Solar Activity and Their Relationship with Solar X-ray,
    Gamma-Emission and Coronal Mass Ejections
Authors: Myagkova, I. N.; Miteva, R.; Kashapova, L.; Bogomolov, A. V.;
   Danov, D.
2019simi.conf..201M    Altcode:
  The study on the relationship of solar cosmic ray events (in
  particular, the ratio of the maximum between the proton and
  electron fluxes) with X-ray and gamma radiation from solar
  flares, as well as with parameters of coronal mass ejections
  was carried out. It was done on the basis of SOHO/ERNE proton
  event catalog (http://newserver.stil.bas.bg/SEPcatalog/)
  and Solar Flares Catalog based on measurements of X- and
  gamma-emission (&gt;50 keV) detected by SONG (CORONAS-F –
  Russian solar observatory) from August, 2001 till December, 2003
  (http://swx.sinp.msu.ru/apps/solar_flares_cat/index.php). Solar electron
  flux (&gt; 300 keV) were measured in the polar caps by MKL-instrument
  on board CORONAS-F satellite.

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Title: About Productivity of the Solar Energetic Particle Events
Authors: Zhdanov, D. A.; Kashapova, L. K.; Myshyakov, I. I.; Miteva, R.
2019simi.conf..211Z    Altcode:
  We present an analysis of 22 SEPs events related to flares that
  demonstrate significant microwave emission. We analyzed the microwave
  burst parameters characterizing acceleration processes for each
  event. In some events, despite the significant microwave signatures,
  powerful SEPs were not produced. <P />The current study aimed to check
  the correlation of the SEP event productivity of active regions based
  on features of their magnetic field topology and the presence of type
  III radio bursts as an additional indicator of open magnetic field
  lines. The magnetic field during the pre-flare stage was extrapolated
  by a potential approximation. The obtained results are discussed.

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Title: Results of work of new spectropolarimeter for solar radio
    emission observations in the range 50-500 MHz
Authors: Muratova, Nataliia; Muratov, Anatoliy; Kashapova, Larisa
2019STP.....5c...3M    Altcode: 2019SZF.....5c...3M
  Ground-based observations within meter radio range are of importance
  for understanding processes occurring in the solar corona. We present
  concepts, block diagram, and results of first observations of the
  Solar Spectropolarimeter of Meter Range (SSMD), launched for solar
  observations in the range 50-500 MHz in April 2016. The main purpose of
  this work was to develop an up-to-date digital radio spectropolarimeter
  able to record the full Stokes vector for sporadic solar phenomena
  taking place in the 50-500 MHz range. We use a crossed log periodic
  antenna to detect solar radio emission. This antenna can simultaneously
  obtain horizontal and vertical polarization components. The main part of
  SSMD is a digital receiver based on an FX correlator architecture. We
  use the Fast Fourier Transform (FFT) algorithm based on the real-time
  pipeline circuit to construct amplitude dynamic spectra (intensity vs
  frequency and time). SSMD has 4608 frequency channels with 97.66 kHz
  channel bandwidth and 97.66 kHz spacing. Time resolution is 1 s. The
  spectropolarimeter has a 50-500 MHz range. It can record the full
  Stokes vector. At present, SSMD observes two of four parameters in
  regular mode (I and V). We have observational data since 2016. The
  catalog development is in progress. We plan to improve time and
  frequency characteristics, record all Stokes parameters, and conduct
  a calibration. We are working on providing access to the data archive
  via the Internet.

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Title: Study on the Features of the SEP Solar Origin Based on
    Microwave Observations
Authors: Kashapova, L. K.; Meshalkina, N. S.; Miteva, R.; Zhukova,
   A. V.; Myagkova, I. N.
2019simi.conf..185K    Altcode:
  We present the results on the analysis of microwave (MW) emission
  in solar flares related to strong solar energetic particle (SEP)
  events observed during the 23rd solar cycle. The parameters of the
  MW spectrum were used as indicators of acceleration processes during
  solar flares. The magnetic topology of the active regions (ARs) that
  produced the flares were taken into account by the approach suggested
  by Abrameko et al. [2018]. We found that during their evolution most
  of the ARs related to proton-rich SEP events violated at least one
  of the classical sunspot group evolution laws (Hale's law, Joy's law
  et cetera). However, the statistical study of all ARs of the cycle
  revealed the domination of normal ARs. The dependences between SEP
  events and MW indicators of the acceleration process for different
  groups are studied and discussed.

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Title: Parameters of Thermal and Non-thermal X-ray and Gamma Ray
    Emission of Solar Flares, Observed onboard CORONAS-F
Authors: Bogomolov, A. V.; Myagkova, I. N.; Miteva, R.; Danov, D.;
   Kashapova, L. K.
2019simi.conf..179B    Altcode:
  Based on data from the SPR-N and SONG multi-channel hard electromagnetic
  radiation detectors onboard the CORONAS-F space observatory and
  the X-ray monitors onboard GOES satellites, we have distinguished
  the thermal and non-thermal components in the X-ray spectrum of a
  number of powerful flares of 23rd solar activity cycle. Temporal,
  spectral and energetic parameters of the flares were analyzed using
  the catalogs of Solar Energetic Particles and Related Phenomena
  (http://newserver.stil.bas.bg/SEPcatalog/).

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Title: Quasi-periodic pulsations in a solar flare with an unusual
    phase shift
Authors: Kupriyanova, Elena G.; Kashapova, Larisa K.; Van Doorsselaere,
   Tom; Chowdhury, Partha; Srivastava, Abhishek K.; Moon, Yong-Jae
2019MNRAS.483.5499K    Altcode: 2018arXiv181209868K; 2018MNRAS.tmp.3312K
  Two kinds of processes could occur during the flare decay
  phase: processes of energy release or processes of energy
  relaxation. Quasi-periodic pulsations (QPPs) of the broad-band
  emission are a good tool for the verification of mechanisms. We aim
  to study the processes during the decay phase of the X-class solar
  flare SOL2014-03-29T17:48. The observations in X-ray, microwave, and
  extreme ultraviolet bands are exploited to study the fine temporal,
  spatial, and spectral structures of the flare. The periods, amplitudes,
  and phases of both the fluxes and physical parameters [emission measure
  (EM), temperature] are studied using standard methods of correlation,
  Fourier, and wavelet analyses. It is found that the source of the QPPs
  is associated with the uniform post-flare loop. The X-ray source is
  located at the top of the arcade. QPPs with the similar characteristic
  time scales of P ≈ 74-80 s are found in the X-ray (3-25 keV) and
  microwave (15.7 GHz) emissions. Besides, QPPs with the same period are
  found in the time profiles of both the temperature (T<SUB>e</SUB>) and
  EM. The QPPs in temperature and the QPPs in EM demonstrate antiphase
  behaviour. The analysis reveals the quasi-periodic process of energy
  relaxation, without any additional source of energy during the decay
  phase. The periods of the QPPs are in a good agreement with second
  harmonic of standing slow magneto-acoustic wave in the arcade that
  could be triggered by a Moreton wave initiated by the flare in the
  direct vicinity of the arcade.

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Title: Onset Time of the GLE 72 Observed at Neutron Monitors and
    its Relation to Electromagnetic Emissions
Authors: Kurt, V.; Belov, A.; Kudela, K.; Mavromichalaki, H.;
   Kashapova, L.; Yushkov, B.; Sgouropoulos, C.
2019SoPh..294...22K    Altcode:
  We present an overview of the ground-level enhancement (GLE 72) of the
  cosmic-ray intensity associated with the recent powerful solar flare
  SOL2017-09-10 (X-ray class X8.9) based on the available neutron monitor
  (NM) network observations and on data from the satellite GOES 13. The
  maximum increase at high-latitude near-sea-level NMs was ≈6 -7 %
  (2-min averages), greater with better time resolution. A scatter plot
  of the maximum increase of the GLE versus solar energetic-particle
  (SEP, proton) flux &gt;100 MeV shows one of the softest spectra
  among GLEs relative to the SEP fluxes. However, at two high-mountain
  middle-latitude NMs the increase was ≈1 % , indicating the possibility
  of proton acceleration up to 6 GeV. Among the analyzed NM data the Fort
  Smith (FSMT) NM shows the earliest and the rather high increase between
  16:06 - 16:08 UT. This indicates an anisotropy in the first phase of
  the GLE event. We calculate the acceptance cones of several NM stations
  at high latitudes and contours of pitch angles corresponding to the
  interplanetary magnetic field (IMF). When employing the available data
  we find that pion-decay γ -ray emission onset is in accordance with the
  time of the main flare energy release. The observed time interval of the
  impulsive burst of &gt;100 MeVγ -ray emission probably corresponds to
  the time of a turbulent current sheet creation. The observed location
  of the impulsive burst pion-decay emission source coincides with the
  active region and the cusp-shaped structure. It seems that models
  assuming sub-relativistic proton production beginning in a turbulent
  reconnecting current sheet are consistent with the observations. If
  these particles were released from the Sun during a type III emission
  with a pion-decay maximum at 16 :00 :30 ±30 UT, we get a plausible
  path length equal to 1.5 ±0.3 AU of the particles responsible for the
  onset of the SEP event and GLE. The time lag of GLE 72 corresponds to
  the most probable interval of the time difference between GLE onset and
  main flare energy release. Although other scenarios are not excluded
  we attribute the protons that create the pion-decay emission and
  the protons responsible for the GLE and SEP event onset to a general
  population of accelerated particles.

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Title: On the role of preflares in tornado-type prominences
Authors: Kupryakov, Yu. A.; Kotrc, P.; Kashapova, L. K.
2019A&AT...31..177K    Altcode:
  We present first results of a study of rotation parameters of the
  tornado-type promi- nences using Hα line spectra and filtergrams. The
  prominences of the tornado-type were observed by ground-based
  spectrographs MFS and HSFA 2 in the Ondrejov Observatory (Astronomical
  Institute of AS CR) from 2000 to 2017. The analysis took into account
  the structure and dynamics of selected prominences and a comparison
  of the data of Hα with the EUV observations of SDO (304 Å, 193 Å,
  171 Å), as well as information about the emission of flares in the
  X-ray range. We found that most of the analyzed events were associated
  with solar flares of classes from B5 to M5 by GOES classification. We
  revealed two types of motions in the prominences. The first type
  shows the Doppler velocity quasi-symmetry of the values in the "blue"
  and "red" Hα line wings. The events of the other type demonstrate
  a difference of up to one order of velocities in the direction of,
  and towards, the observer.

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Title: Characteristics of SEP Events and Their Solar Origin During
    the Evolution of Active Region NOAA 10069
Authors: Kashapova, L. K.; Miteva, R.; Myagkova, I. N.; Bogomolov,
   A. V.
2019SoPh..294....9K    Altcode:
  We present the results of a comparative analysis of the properties of
  a series of successive solar flares, which occurred in active region
  (AR) 10069 in August 2002, and the associated solar energetic particle
  (SEP) events. The active region was extremely flare productive
  during its evolution. The solar flare characteristics are based on
  X-ray and radio emission data: maximum detected photon energies and
  spectral index, delays between microwave, metric-radio and, hard
  X-ray emissions. The coronal mass ejections (CMEs) are characterized
  by their projected speed. The SEP properties are described by the
  relative electron to proton abundance as well as by the abundance of
  lower relative to higher energy particles. The analysis carried out
  supports some previous results obtained by large statistical studies,
  but at the same time refutes others. For example, the set of analyzed
  events that occurred in the AR did not show clear evidence of the big
  flare syndrome though the large proton events observed near Earth were
  always accompanied by CMEs. Some of the peculiar observations could
  be the result of the magnetic topology of the AR.

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Title: Comparative analysis of the proton generation efficiency
    during 17 March 2003 and 11 April 2004 solar flares
Authors: Bogomolov, A. V.; Myagkova, I. N.; Myshyakov, I.; Tsvetkov,
   Ts; Kashapova, L.; Miteva, R.
2018JASTP.179..517B    Altcode:
  We present the comparative analysis of the solar energetic particle
  (SEP) event properties and the indicators of acceleration processes
  in solar flares - the hard X-rays (HXR) and radio emission from
  microwaves to the meter-range. We focus our study on the two SEP
  events associated with solar flares with similar characteristics in
  HXR emission and the close location on solar disk. The proton flux
  in the SEP event associated with the weaker flare by GOES class in
  soft X-ray (SXR) (C9.6/SOL2004-Apr-11) was more than an order higher
  than in the SEP event associated with the more powerful solar flare
  (X1.5/SOL2003-Mar-17). At the same time, the electron fluxes in both SEP
  events were comparable. Both flares were followed by CMEs with speed
  above 1000 km s<SUP>-1</SUP>. The analysis of SEP fluxes and flare
  plasma parameters was done taking into account the magnetic topology
  of the active region (AR) and its evolution before and during the
  solar flares. The 3D reconstruction of the potential magnetic field
  showed the existence of an arcade of high loops covering the active
  region where the more powerful flare occurred. The flare associated
  with the proton-rich SEP event occurred in the active region where
  3D reconstruction revealed a fan of high loops associated with open
  magnetic field lines. We suppose that the arcade of high loops could be
  the factor which prevents an escape of the accelerated particles into
  the interplanetary space (IPS) while the fan of high loops facilitates
  the production of the more proton-rich SEP events. Results of the
  analysis show a necessity to use topology of ARs as a parameter in
  statistical studies of SEP event origins.

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Title: Radio, Hard X-Ray, and Gamma-Ray Emissions Associated with
    a Far-Side Solar Event
Authors: Grechnev, V. V.; Kiselev, V. I.; Kashapova, L. K.; Kochanov,
   A. A.; Zimovets, I. V.; Uralov, A. M.; Nizamov, B. A.; Grigorieva,
   I. Y.; Golovin, D. V.; Litvak, M. L.; Mitrofanov, I. G.; Sanin, A. B.
2018SoPh..293..133G    Altcode: 2018arXiv180810103G
  The far-side solar eruptive event SOL2014-09-01 produced hard
  electromagnetic and radio emissions that were observed with detectors at
  near-Earth vantage points. Especially challenging was a long-duration
  &gt; 100 MeV γ -ray burst that was probably produced by accelerated
  protons exceeding 300 MeV. This observation raised the question how
  high-energy protons could reach the Earth-facing solar surface. Some
  preceding studies discussed a scenario in which protons accelerated by a
  shock driven by a coronal mass ejection high in the corona return to the
  solar surface. We continue with the analysis of this challenging event,
  involving radio images from the Nançay Radioheliograph and hard X-ray
  data from the High Energy Neutron Detector (HEND) of the Gamma-Ray
  Spectrometer onboard the Mars Odyssey space observatory located near
  Mars. HEND recorded unocculted flare emission. The results indicate
  that the emissions observed from the Earth's direction were generated by
  flare-accelerated electrons and protons trapped in static long coronal
  loops. They can be reaccelerated in these loops by a shock wave that was
  excited by the eruption, being initially not driven by a coronal mass
  ejection. The results highlight ways to address the remaining questions.

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Title: Multi-instrument view on solar eruptive events observed with
the Siberian Radioheliograph: From detection of small jets up to
    development of a shock wave and CME
Authors: Grechnev, V. V.; Lesovoi, S. V.; Kochanov, A. A.; Uralov,
   A. M.; Altyntsev, A. T.; Gubin, A. V.; Zhdanov, D. A.; Ivanov, E. F.;
   Smolkov, G. Ya.; Kashapova, L. K.
2018JASTP.174...46G    Altcode: 2018arXiv180502564G
  The first 48-antenna stage of the Siberian Radioheliograph (SRH)
  started single-frequency test observations early in 2016, and since
  August 2016 it routinely observes the Sun at several frequencies in
  the 4-8 GHz range with an angular resolution of 1-2 arc minutes and
  an imaging interval of about 12 s. With limited opportunities of the
  incomplete antenna configuration, a high sensitivity of about 100
  Jy allows the SRH to contribute to the studies of eruptive phenomena
  along three lines. First, some eruptions are directly visible in SRH
  images. Second, some small eruptions are detectable even without a
  detailed imaging information from microwave depressions caused by
  screening the background emission by cool erupted plasma. Third,
  SRH observations reveal new aspects of some events to be studied
  with different instruments. We focus on an eruptive C2.2 flare on
  16 March 2016 around 06:40, one of the first flares observed by the
  SRH. Proceeding from SRH observations, we analyze this event using
  extreme-ultraviolet, hard X-ray, white-light, and metric radio data. An
  eruptive prominence expanded, brightened, and twisted, which indicates
  a time-extended process of the flux-rope formation together with the
  development of a large coronal mass ejection (CME). The observations
  rule out a passive role of the prominence in the CME formation. The
  abrupt prominence eruption impulsively excited a blast-wave-like
  shock, which appeared during the microwave burst and was manifested
  in an "EUV wave" and Type II radio burst. The shock wave decayed and
  did not transform into a bow shock because of the low speed of the
  CME. Nevertheless, this event produced a clear proton enhancement near
  Earth. Comparison with our previous studies of several events confirms
  that the impulsive-piston shock-excitation scenario is typical of
  various events.

---------------------------------------------------------
Title: Results of comparative analysis of the SEP events and the
    microwave bursts observed by 2-24 GHz and 4-8 GHz spectropolarimeters
    in 2010-2016
Authors: Zhdanov, D.; Kashapova, L. K.; Miteva, R.
2018simi.conf..105Z    Altcode:
  We present a relationship analysis between the solar energetic particle
  (SEP) events and the microwave (MW) spectral observations of the solar
  bursts detected in 2010-2016. The information about the SEP events
  is taken from the Wind/EPACT catalog based on data in the period
  1996-2016. We use MW data from the archive of MW observations in the
  range 2-24 GHz. Observations were made by spectropolarimeters of the
  SSRT observatory (Russia). We found that 40 events are present in both
  catalogs. We tested the relationships between the proton spectral index
  of SEP events and the peak frequency of the MW bursts and presence of
  circular polarization in MW emission of selected events. The results
  are finally discussed.

---------------------------------------------------------
Title: Analysing of the SEP origins based on microwave emission of
    solar flares
Authors: Kashapova, L.; Mehsalkina, N.; Miteva, R.; Myagkova, I.;
   Bogomolov, A.
2018simi.conf..119K    Altcode:
  We present the results on the analysis of microwave emission in
  solar flares related to strong solar energetic particle (SEP) events
  observed during the previous solar cycle. The target of the work is
  to find criteria based on the solar flare features that would allow
  us to separate the SEP events into groups with more homogeneous
  physical/topological properties. In the current study, we compared
  peak frequency of microwave spectra and spectral index with spectral
  characteristics of SEP proton fluxes. The two groups of events related
  to the value of the peak frequency are found. We discuss revealed
  tendencies and physical reasons of the two population appearances.

---------------------------------------------------------
Title: The efficiency of solar energetic particle generation:
    CORONAS-F mission data analysis
Authors: Myagkova, I. N.; Miteva, R.; Kashapova, L.; Bogomolov, A. V.;
   Petrov, V.; Tsvetkov, Ts.; Meshalkina, N.; Myshyakov, I.
2018simi.conf..114M    Altcode:
  We present the results of a comparative analysis on the efficiency
  of the solar energetic particle events (SEP) and related solar
  flares. Both SEP events and solar flares were detected by the CORONAS-F
  solar mission. We selected the SEP events based on the presence of
  simultaneous observations from the hard X-ray (HXR) instrument SONG
  (CORONAS-F satellite) with radio emission ranging from microwaves
  to the meter-range, as evidence of accelerated particles generated
  during the events and solar proton and electron data measured by MKL
  instrument on board CORONAS-F satellite in polar caps. The results
  are discussed from point of using solar flare emission features as
  the criteria of generation of SEP event with high proton abundance.

---------------------------------------------------------
Title: Homologous Circular-ribbon Flares Driven by Twisted Flux
    Emergence
Authors: Xu, Z.; Yang, K.; Guo, Y.; Zhao, J.; Zhao, Z. J.; Kashapova,
   L.
2017ApJ...851...30X    Altcode:
  In this paper, we report two homologous circular-ribbon flares
  associated with two filament eruptions. They were well observed by the
  New Vacuum Solar Telescope and the Solar Dynamics Observatory on 2014
  March 5. Prior to the flare, two small-scale filaments enclosed by a
  circular pre-flare brightening lie along the circular polarity inversion
  line around the parasitic polarity, which has shown a continuous
  rotation since its first appearance. Two filaments eventually erupt
  in sequence associated with two homologous circular-ribbon flares and
  display an apparent writhing signature. Supplemented by the nonlinear
  force-free field extrapolation and the magnetic field squashing factor
  investigation, the following are revealed. (1) This event involves
  the emergence of magnetic flux ropes into a pre-existing polarity
  area, which yields the formation of a 3D null-point topology in
  the corona. (2) Continuous input of the free energy in the form of
  a flux rope from beneath the photosphere may drive a breakout-type
  reconnection occurring high in the corona, supported by the pre-flare
  brightening. (3) This initiation reconnection could release the
  constraint on the flux rope and trigger the MHD instability to first
  make filament F1 lose equilibrium. The subsequent more violent magnetic
  reconnection with the overlying flux is driven during the filament
  rising. In return, the eruption of filament F2 is further facilitated by
  the reduction of the magnetic tension force above. These two processes
  form a positive feedback to each other to cause the energetic mass
  eruption and flare.

---------------------------------------------------------
Title: The origin of SEP events: New research collaboration and
    network on space weather
Authors: Miteva, Rositsa; Kashapova, Larisa; Myagkova, Irina;
   Meshalkina, Nataliia; Petrov, Nikola; Bogomolov, Andrey; Myshyakov,
   Ivan; Tsvetkov, Tsvetan; Danov, Dimitar; Zdanov, Dmitriy
2017ses..conf...57M    Altcode:
  A new project on the solar energetic particles (SEPs) and their solar
  origins (flares and coronal mass ejections) is described here. The
  main aim of this project is to answer the question - whether the SEPs
  observed in situ are driven by flares, by CMEs or both accelerators
  contribute to an extent which varies from event to event - by deducing
  a quantitative measure of the flare vs. CME contribution, duration
  and efficiency. New observations (SONG/Koronas-F, Relec/Vernov) and
  new approaches of analysis will be utilized (e.g., magnetic topology
  of active regions using 3D extrapolation techniques of detailed
  case studies together with statistical analysis of the phenomena). In
  addition, the identification of the uncertainty limits of SEP injection,
  onset time and testing the validity of assumptions often taken for
  granted (association procedures, solar activity longitudinal effects,
  correlation analysis, etc.) are planned. The project outcomes have
  the capacity to contribute to other research fields for improvement
  of modeling schemes and forecasting methods of space weather events.

---------------------------------------------------------
Title: CORONAS-F observation of gamma-ray emission from the solar
    flare on 2003 October 29
Authors: Kurt, Victoria G.; Yushkov, Boris Yu.; Galkin, Vladimir I.;
   Kudela, Karel; Kashapova, Larisa K.
2017NewA...56..102K    Altcode: 2018arXiv180802627K
  Appreciable hard X-ray (HXR) and gamma-ray emissions in the 0.04-150 MeV
  energy range associated with the 2003 October 29 solar flare (X10/3B)
  were observed at 20:38-20:58 UT by the SONG instrument onboard the
  CORONAS-F mission. To restore flare gamma-ray spectra we fitted the
  SONG energy loss spectra with a three-component model of the incident
  spectrum: (1) a power law in energy, assumed to be due to electron
  bremsstrahlung; (2) a broad continuum produced by prompt nuclear
  de-excitation gamma-lines; and (3) a broad gamma-line generated from
  pion-decay. We also restored spectra from the RHESSI data, compared
  them with the SONG spectra and found a reasonable agreement between
  these spectra in the 0.1-10 MeV energy range. The pion-decay emission
  was observed from 20:44:20 UT and had its maximum at 20:48-20:51 UT. The
  power-law spectral index of accelerated protons estimated from the ratio
  between intensities of different components of gamma rays changed with
  time. The hardest spectrum with a power-law index S = -3.5 - 3.6 was
  observed at 20:48-20:51 UT. Time histories of the pion-decay emission
  and proton spectrum were compared with changes of the locations
  of flare energy release as shown by RHESSI hard X-ray images and
  remote and remote Hα brightenings. An apparent temporal correlation
  between processes of particle acceleration and restructuring of flare
  magnetic field was found. In particular, the protons were accelerated
  to subrelativistic energies after radical change of the character of
  footpoint motion from a converging motion to a separation motion.

---------------------------------------------------------
Title: Siberian Radioheliograph: first results
Authors: Lesovoi, Sergey; Altyntsev, Alexander; Kochanov, Aleksey;
   Grechnev, Victor; Gubin, Aleksey; Zhdanov, Dmitriy; Ivanov, Evgeniy;
   Uralov, Arkadiy; Kashapova, Larisa; Kuznetsov, Aleksey; Meshalkina,
   Nataliya; Sych, Robert
2017STP.....3a...3L    Altcode: 2017SZF.....3a...3L; 2017arXiv170407100L
  Regular observations of active processes in the solar atmosphere
  have been started using the first stage of the multiwave Siberian
  Radioheliograph (SRH), a T-shaped 48-antenna array with a 4-8 GHz
  operating frequency range and a 10 MHz instantaneous receiving
  band. Antennas are mounted on the central antenna posts of the
  Siberian Solar Radio Telescope. The maximum baseline is 107.4 m,
  and the angular resolution is up to 70". We present examples of
  observations of the solar disk at different frequencies, "negative"
  bursts, and solar flares. The sensitivity to compact sources reaches
  0.01 solar flux units (≈10<SUP>-4</SUP> of the total solar flux)
  with an accumulation time of about 0.3 s. The high sensitivity of
  SRH enables monitoring of solar activity and allows studying active
  processes from characteristics of their microwave emission, including
  faint events, which could not be detected previously.

---------------------------------------------------------
Title: Fermi-LAT Observations of High-energy Behind-the-limb Solar
    Flares
Authors: Ackermann, M.; Allafort, A.; Baldini, L.; Barbiellini, G.;
   Bastieri, D.; Bellazzini, R.; Bissaldi, E.; Bonino, R.; Bottacini, E.;
   Bregeon, J.; Bruel, P.; Buehler, R.; Cameron, R. A.; Caragiulo, M.;
   Caraveo, P. A.; Cavazzuti, E.; Cecchi, C.; Charles, E.; Ciprini, S.;
   Costanza, F.; Cutini, S.; D'Ammando, F.; de Palma, F.; Desiante, R.;
   Digel, S. W.; Di Lalla, N.; Di Mauro, M.; Di Venere, L.; Drell, P. S.;
   Favuzzi, C.; Fukazawa, Y.; Fusco, P.; Gargano, F.; Giglietto, N.;
   Giordano, F.; Giroletti, M.; Grenier, I. A.; Guillemot, L.; Guiriec,
   S.; Jogler, T.; Jóhannesson, G.; Kashapova, L.; Krucker, S.; Kuss,
   M.; La Mura, G.; Larsson, S.; Latronico, L.; Li, J.; Liu, W.; Longo,
   F.; Loparco, F.; Lubrano, P.; Magill, J. D.; Maldera, S.; Manfreda,
   A.; Mazziotta, M. N.; Mitthumsiri, W.; Mizuno, T.; Monzani, M. E.;
   Morselli, A.; Moskalenko, I. V.; Negro, M.; Nuss, E.; Ohsugi, T.;
   Omodei, N.; Orlando, E.; Pal'shin, V.; Paneque, D.; Perkins, J. S.;
   Pesce-Rollins, M.; Petrosian, V.; Piron, F.; Principe, G.; Rainò,
   S.; Rando, R.; Razzano, M.; Reimer, O.; Rubio da Costa, F.; Sgrò,
   C.; Simone, D.; Siskind, E. J.; Spada, F.; Spandre, G.; Spinelli,
   P.; Tajima, H.; Thayer, J. B.; Torres, D. F.; Troja, E.; Vianello, G.
2017ApJ...835..219A    Altcode: 2017arXiv170200577A
  We report on the Fermi-LAT detection of high-energy emission from the
  behind-the-limb (BTL) solar flares that occurred on 2013 October 11,
  and 2014 January 6 and September 1. The Fermi-LAT observations are
  associated with flares from active regions originating behind both
  the eastern and western limbs, as determined by STEREO. All three
  flares are associated with very fast coronal mass ejections (CMEs)
  and strong solar energetic particle events. We present updated
  localizations of the &gt;100 MeV photon emission, hard X-ray (HXR)
  and EUV images, and broadband spectra from 10 keV to 10 GeV, as well
  as microwave spectra. We also provide a comparison of the BTL flares
  detected by Fermi-LAT with three on-disk flares and present a study
  of some of the significant quantities of these flares as an attempt
  to better understand the acceleration mechanisms at work during these
  occulted flares. We interpret the HXR emission to be due to electron
  bremsstrahlung from a coronal thin-target loop top with the accelerated
  electron spectra steepening at semirelativistic energies. The &gt;100
  MeV gamma-rays are best described by a pion-decay model resulting
  from the interaction of protons (and other ions) in a thick-target
  photospheric source. The protons are believed to have been accelerated
  (to energies &gt;10 GeV) in the CME environment and precipitate down to
  the photosphere from the downstream side of the CME shock and landed
  on the front side of the Sun, away from the original flare site and
  the HXR emission.

---------------------------------------------------------
Title: Fermi Large Area Telescope Observations of High-Energy
    Gamma-ray Emission From Behind-the-limb Solar Flares
Authors: Omodei, Nicola; Pesce-Rollins, Melissa; Petrosian, Vahe;
   Liu, Wei; Rubio da Costa, Fatima; Golenetskii, Sergei; Kashapova,
   Larisa; Krucker, Sam; Palshin, Valentin; Fermi Large Area Telescope
   Collaboration
2017APS..APR.Y3005O    Altcode:
  Fermi LAT &gt;30 MeV observations of the active Sun have increased
  the number of detected solar flares by almost a factor of 10 with
  respect to previous space observations. Of particular interest are the
  recent detections of three solar flares whose position behind the limb
  was confirmed by the STEREO-B spacecraft. These observations sample
  flares from active regions originating from behind both the eastern
  and western limbs and include an event associated with the second
  ground level enhancement event (GLE) of the 24th Solar Cycle. While
  gamma-ray emission up to tens of MeV resulting from proton interactions
  has been detected before from occulted solar flares, the significance
  of these particular events lies in the fact that these are the first
  detections of &gt;100 MeV gamma-ray emission from footpoint-occulted
  flares. These detections present an unique opportunity to diagnose
  the mechanisms of high-energy emission and particle acceleration and
  transport in solar flares. We will present the Fermi-LAT, RHESSI and
  STEREO observations of these flares and discuss the various emission
  scenarios for these sources.

---------------------------------------------------------
Title: Solar X-ray Emission Measured by the Vernov Mission During
    September - October of 2014
Authors: Myagkova, I. N.; Bogomolov, A. V.; Kashapova, L. K.;
   Bogomolov, V. V.; Svertilov, S. I.; Panasyuk, M. I.; Kuznetsova,
   E. A.; Rozhkov, G. V.
2016SoPh..291.3439M    Altcode: 2016SoPh..tmp..128M
  Solar hard X-ray and γ -ray emissions were measured by the Detector
  of the Roentgen and Gamma-ray Emissions (DRGE) instrument, which is
  part of the RELEC set of instruments operated onboard the Russian
  satellite Vernov, from July 8, 2014 until December 10, 2014 (on a
  solar-synchronous orbit with an apogee of 830 km, perigee of 640 km,
  and an inclination of 98.4<SUP>∘</SUP>). RELEC measurements of 18
  flares with X-ray energy &gt;30 keV, taken in September - October
  2014, were connected with the same active region with the number AR
  12172 during the first rotation and AR 12192 during the next one. These
  measurements were compared to the data obtained with RHESSI, Konus-Wind,
  Fermi Observatory, Radio Solar Telescope Net (RSTN), and the Nobeyama
  Radioheliograph (NoRH) operating at the same time. Quasi-periodicities
  with similar periods of 7 ±2 s were found in about one third of all
  flares measured by RELEC (Vernov) from September 24 until October
  30, 2014.

---------------------------------------------------------
Title: Relationship of Type III Radio Bursts with Quasi-periodic
    Pulsations in a Solar Flare
Authors: Kupriyanova, E. G.; Kashapova, L. K.; Reid, H. A. S.;
   Myagkova, I. N.
2016SoPh..291.3427K    Altcode: 2016arXiv160800129K; 2016SoPh..tmp..127K
  We studied a solar flare with pronounced quasi-periodic pulsations
  detected in the microwave, X-ray, and radio bands. We used correlation,
  Fourier, and wavelet analyses methods to examine the temporal fine
  structures and relationships between the time profiles in each wave
  band. We found that the time profiles of the microwaves, hard X-rays,
  and type III radio bursts vary quasi-periodically with a common period
  of 40 - 50 s. The average amplitude of the variations is high, above
  30 % of the background flux level, and reaches 80 % after the flare
  maximum. We did not find this periodicity in either the thermal X-ray
  flux component or in the source size dynamics. Our findings indicate
  that the detected periodicity is probably associated with periodic
  dynamics in the injection of non-thermal electrons, which can be
  produced by periodic modulation of magnetic reconnection.

---------------------------------------------------------
Title: Diagnosing the Source Region of a Solar Burst on 26 September
    2011 by Using Microwave Type-III Pairs
Authors: Tan, B. L.; Karlický, M.; Mészárosová, H.; Kashapova,
   L.; Huang, J.; Yan, Y.; Kontar, E. P.
2016SoPh..291.2407T    Altcode: 2016SoPh..tmp..143T; 2016arXiv160605410T
  We report a peculiar and interesting train of microwave Type-III pair
  bursts in the impulsive rising phase of a solar flare on 26 September
  2011. The observations include radio spectrometers at frequencies
  of 0.80 - 2.00 GHz from the Ondřejov radiospectrograph in the
  Czech Republic (ORSC), hard X-ray from the Ramaty High-Energy Solar
  Spectroscopic Imager (RHESSI) and Gamma-Ray Burst Monitor onboard
  the Fermi Space Telescope (Fermi/GRB), EUV images from the Sun
  Watcher using APS detectors and image Processing instrument onboard
  the Project for Onboard Autonomy 2 (SWAP/PROBA2), and magnetograms
  from the Helioseismic and Magnetic Imager onboard the Solar Dynamic
  Observatory (SDO/HMI). By using a recently developed method (Tan et al.,
  Res. Astron. Astrophys.16, 82, 2016a), we diagnosed the plasma density,
  temperature, plasma-β , magnetic field near the source region, the
  energy of energetic electrons, and the distance between the acceleration
  region and the emission start sites of Type-III bursts. From the
  diagnostics, we find that i) The plasma density, temperature, magnetic
  field, and the distance between the acceleration region and the emission
  start sites have almost no obvious variations during the period of
  Type-III pair trains, while the energy of electrons has an obvious
  peak value that is consistent with the hard X-ray emission. ii) The
  plasma-β is much higher than unity, showing a highly dynamic process
  near the emission start site of Type-III bursts. iii) Although the
  reversed-slope Type-III branches drift more slowly by one order of
  magnitude than that of the normal Type-IIIs, the related descending
  and ascending electrons still could have energy of the same order of
  magnitude. These facts indicate that both the ascending and descending
  electrons are possibly accelerated by a similar mechanism and in a
  small source region. These diagnostics can help us to understand the
  physics in the source region of solar bursts.

---------------------------------------------------------
Title: Broadband microwave sub-second pulsations in an expanding
    coronal loop of the 2011 August 10 flare
Authors: Mészárosová, H.; Rybák, J.; Kashapova, L.; Gömöry,
   P.; Tokhchukova, S.; Myshyakov, I.
2016A&A...593A..80M    Altcode: 2016arXiv160904217M
  <BR /> Aims: We studied the characteristic physical properties and
  behavior of broadband microwave sub-second pulsations observed in
  an expanding coronal loop during the GOES C2.4 solar flare on 2011
  August 10. <BR /> Methods: The complex microwave dynamic spectrum and
  the expanding loop images were analyzed with the help of SDO/AIA/HMI,
  RHESSI, and the STEREO/SECCHI-EUVI data processing software, wavelet
  analysis methods, the GX Simulator tool, and the NAFE method. <BR />
  Results: We found sub-second pulsations and other different burst
  groups in the complex radio spectrum. The broadband (bandwidth about
  1 GHz) sub-second pulsations (temporal period range 0.07-1.49 s,
  no characteristic dominant period) lasted 70 s in the frequency
  range 4-7 GHz. These pulsations were not correlated at their
  individual frequencies, had no measurable frequency drift, and zero
  polarization. In these pulsations, we found the signatures of fast
  sausage magnetoacoustic waves with the characteristic periods of 0.7
  and 2 s. The other radio bursts showed their characteristic frequency
  drifts in the range of -262-520 MHz s<SUP>-1</SUP>. They helped us to
  derive average values of 20-80 G for the coronal magnetic field strength
  in the place of radio emission. It was revealed that the microwave
  event belongs to an expanding coronal loop with twisted sub-structures
  observed in the 131, 94, and 193 Å SDO/AIA channels. Their slit-time
  diagrams were compared with the location of the radio source at 5.7 GHz
  to realize that the EUV intensity of the expanding loop increased just
  before the radio source triggering. We reveal two EUV bidirectional
  flows that are linked with the start time of the loop expansion. Their
  positions were close to the radio source and propagated with velocities
  within a range of 30-117 km s<SUP>-1</SUP>. <BR /> Conclusions: We
  demonstrate that periodic regime of the electron acceleration in a model
  of the quasi-periodic magnetic reconnection might be able to explain
  physical properties and behavior of the sub-second pulsations. The
  depolarization process of the microwave emission might be caused by
  a plasma turbulence in the radio source. Finally, the observed EUV
  flows might be linked with reconnection outflows.

---------------------------------------------------------
Title: Time delays in the nonthermal radiation of solar flares
    according to observations of the CORONAS-F satellite
Authors: Tsap, Yu. T.; Stepanov, A. V.; Kashapova, L. K.; Myagkova,
   I. N.; Bogomolov, A. V.; Kopylova, Yu. G.; Goldvarg, T. B.
2016CosRe..54..285T    Altcode:
  In 2001-2003, the X-ray and microwave observations of ten solar flares
  of M- and X-classes were carried out by the CORONAS-F orbital station,
  the RSTN Sun service, and Nobeyama radio polarimeters. Based on these
  observations, a correlation analysis of time profiles of nonthermal
  radiation was performed. On average, hard X-ray radiation outstrips the
  microwave radiation in 9 events, i.e., time delays are positive. The
  appearance of negative delays is associated with effective scattering
  of accelerated electrons in pitch angles, where the length of the free
  path of a particle is less than the half-length of a flare loop. The
  additional indications are obtained in favor of the need to account for
  the effect of magnetic mirrors on the dynamics of energetic particles
  in the coronal arches.

---------------------------------------------------------
Title: A Cold Flare with Delayed Heating
Authors: Fleishman, Gregory D.; Pal'shin, Valentin D.; Meshalkina,
   Natalia; Lysenko, Alexandra L.; Kashapova, Larisa K.; Altyntsev,
   Alexander T.
2016ApJ...822...71F    Altcode: 2016arXiv160307273F
  Recently, a number of peculiar flares have been reported that
  demonstrate significant nonthermal particle signatures with low,
  if any, thermal emission, which implies a close association of the
  observed emission with the primary energy release/electron acceleration
  region. This paper presents a flare that appears “cold” at the
  impulsive phase, while displaying delayed heating later on. Using
  hard X-ray data from Konus-Wind, microwave observations by SSRT, RSTN,
  NoRH, and NoRP, context observations, and three-dimensional modeling,
  we study the energy release, particle acceleration, and transport, and
  the relationships between the nonthermal and thermal signatures. The
  flaring process is found to involve the interaction between a small
  loop and a big loop with the accelerated particles divided roughly
  equally between them. Precipitation of the electrons from the small loop
  produced only a weak thermal response because the loop volume was small,
  while the electrons trapped in the big loop lost most of their energy in
  the coronal part of the loop, which resulted in coronal plasma heating
  but no or only weak chromospheric evaporation, and thus unusually
  weak soft X-ray emission. The energy losses of the fast electrons in
  the big tenuous loop were slow, which resulted in the observed delay
  of the plasma heating. We determined that the impulsively accelerated
  electron population had a beamed angular distribution in the direction
  of the electric force along the magnetic field of the small loop. The
  accelerated particle transport in the big loop was primarily mediated
  by turbulent waves, which is similar to other reported cold flares.

---------------------------------------------------------
Title: A Tiny Eruptive Filament as a Flux-Rope Progenitor and Driver
    of a Large-Scale CME and Wave
Authors: Grechnev, V. V.; Uralov, A. M.; Kochanov, A. A.; Kuzmenko,
   I. V.; Prosovetsky, D. V.; Egorov, Y. I.; Fainshtein, V. G.; Kashapova,
   L. K.
2016SoPh..291.1173G    Altcode: 2016SoPh..tmp...57G; 2016arXiv160400800G
  A solar eruptive event SOL2010-06-13 observed with the Atmospheric
  Imaging Assembly (AIA) of the Solar Dynamics Observatory (SDO) has been
  extensively discussed in the contexts of the CME development and an
  associated extreme-ultraviolet (EUV) wave-like transient in terms of a
  shock driven by the apparent CME rim. Continuing the analysis of this
  event, we have revealed an erupting flux rope, studied its properties,
  and detected wave signatures inside the developing CME. These findings
  have allowed us to establish new features in the genesis of the CME and
  associated EUV wave and to reconcile all of the episodes into a single
  causally related sequence. i) A hot 11 MK flux rope developed from the
  structures initially associated with a compact filament system. The flux
  rope expanded with an acceleration of up to 3 km s<SUP>−2</SUP> one
  minute before a hard X-ray burst and earlier than any other structures,
  reached a velocity of 420 km s<SUP>−1</SUP>, and then decelerated
  to about 50 km s<SUP>−1</SUP>. ii) The CME development was driven
  by the expanding flux rope. Closed coronal structures above the rope
  got sequentially involved in the expansion from below upwards, came
  closer together, and apparently disappeared to reveal their common
  envelope, the visible rim, which became the outer boundary of the
  cavity. The rim was probably associated with the separatrix surface of
  a magnetic domain, which contained the pre-eruptive filament. iii) The
  rim formation was associated with a successive compression of the upper
  active-region structures into the CME frontal structure (FS). When the
  rim was formed, it resembled a piston. iv) The disturbance responsible
  for the consecutive CME formation episodes was excited by the flux rope
  inside the rim, and then propagated outward. EUV structures arranged
  at different heights started to accelerate, when their trajectories
  in the distance-time diagram were crossed by that of the fast front of
  this disturbance. v) Outside the rim and FS, the disturbance propagated
  like a blast wave, manifesting in a type II radio burst and a leading
  part of the EUV transient. Its main, trailing part was the FS, which
  consisted of swept-up 2 MK coronal loops enveloping the expanding
  rim. The wave decelerated and decayed into a weak disturbance soon
  afterwards, being not driven by the trailing piston, which slowed down.

---------------------------------------------------------
Title: Sunspot waves and flare energy release
Authors: Sych, R.; Karlický, M.; Altyntsev, A.; Dudík, J.;
   Kashapova, L.
2015A&A...577A..43S    Altcode: 2014arXiv1409.2947S
  Context. We study the possibility of flare process triggering by
  waves propagating from the sunspot along a magnetic loop (channel)
  to a nearby flare site. <BR /> Aims: We present a relationship between
  the dynamics of ~3-min slow magnetoacoustic waves in the sunspot and
  flare emergence process. Waves propagating in the magnetic channel
  whose one foot is anchored in the umbra represent the disturbing agent
  responsible for triggering the flare energy release. <BR /> Methods:
  We applied time-distance plots and pixel wavelet filtration methods
  to obtain spatio-temporal distribution of wave power variations in
  radio and SDO/AIA data. To find the magnetic channel, we used potential
  magnetic field extrapolation of SDO/HMI magnetograms. The propagation
  velocity of wave fronts was measured from wave locations at specific
  times. <BR /> Results: In the correlation curves of the 17 GHz (NoRH)
  radio emission, we found a monotonous energy amplification of the
  3-min waves in the sunspot umbra before the 2012 June 7 flare. This
  amplification was associated with an increase in the length of the
  oscillatory wakes in coronal loops (SDO/AIA, 171 Å) prior to the flare
  onset. A peculiarity of the flare is the constant level of the flare
  emission in soft X-rays (RHESSI, 3-25 keV) for ~10 min after the short
  impulsive phase, which indicates continuing energy release. Throughout
  this time, we found transverse oscillations of the flare loop with a
  30 s period in the radio-frequency range (NoRH, 17 GHz). This period
  appears to be related to the 3-min waves from the sunspot. The magnetic
  field extrapolation based on SDO/HMI magnetograms shows the existence
  of the magnetic channel (waveguide) connecting the sunspot with the
  energy release region. <BR /> Conclusions: We analysed the sunspot
  3-min wave dynamics and found a correlation between the oscillation
  power amplification and flare triggering in the region connected to the
  sunspot through the magnetic channel. We propose that this amplified
  wave flux triggered the flare. The flare occurred because of this
  amplified flux, however, and because a sufficient amount of free
  magnetic energy was accumulated in close vicinity to the magnetic
  channel prior to the flare. Furthermore, because of loop heating,
  the wave velocity (sound velocity) increased with the penetration of
  waves into the energy release site. The heating is shown to be able to
  proceed after the flare main peak owing to a further energy pumping
  in the form of waves from the sunspot and additional reconnection
  episodes in the flare region.

---------------------------------------------------------
Title: CORONAS-F observation of HXR and gamma-ray emissions from
    the solar flare X10 on 29 October 2003 as a probe of accelerated
    proton spectrum
Authors: Kurt, V. G.; Yushkov, B. Yu.; Kudela, K.; Galkin, V. I.;
   Kashapova, L. K.
2015CoSka..45...42K    Altcode:
  HXR and gamma-ray emissions in the 0.04—150 MeV energy range
  associated with the solar flare on 29 October 2003 (X10/3B) were
  observed at 20:38—20:58 UT by the SONG instrument aboard the CORONAS-F
  mission. We restored consecutive flare gamma-emission spectra from
  SONG and RHESSI data and found a good agreement of these spectra in
  the 0.1—10 MeV energy range. Two phases were identified which showed
  major changes in the spectral shape of flare emission: 20:38:00-20:44:20
  UT and 20:44:20-20:58:00 UT. During the second phase an efficiency of
  proton acceleration increased considerably relatively to the efficiency
  of acceleration of high energy electrons. The pion-decay component of
  the flare gamma-emission was elicited statistically significant only
  during the second phase since 20:47:40 UT. A power law spectrum index of
  accelerated protons was estimated from the ratio between intensities of
  the pion-decay and gamma-line components. The hardest spectrum (power
  law index S=3.7) was at 20:48—20:51 UT when the intensity of the
  pion-decay emission was maximal. Our subdivision of the flare into two
  phases is consistent with sharp changes in the structure of the flare
  found by Ji et al. (2008) and Liu et al. (2009). <P />This flare was
  accompanied by GLE 66. The time profile of the pion-decay gamma-emission
  was compared with the GLE onset time. It was shown that both protons
  interacting at the Sun and the particles responsible for the GLE onset
  could belong to the same population of accelerated particles.

---------------------------------------------------------
Title: Editorial: solar radiophysics — recent results on
    observations and theories
Authors: Nakariakov, Valery M.; Kashapova, Larisa K.; Yan, Yi-Hua
2014RAA....14....1N    Altcode:
  Solar radiophysics is a rapidly developing branch of solar physics
  and plasma astrophysics. Solar radiophysics has the goal of analyzing
  observations of radio emissions from the Sun and understanding basic
  physical processes operating in quiet and active regions of the solar
  corona. In the near future, the commissioning of a new generation
  of solar radio observational facilities, which include the Chinese
  Spectral Radio Heliograph (CSRH) and the upgrade of the Siberian
  Solar Radio Telescope (SSRT), and the beginning of solar observations
  with the Atacama Large Millimeter/submillimeter Array (ALMA), is
  expected to bring us new breakthrough results of a transformative
  nature. The Marie-Curie International Research Staff Exchange (MC
  IRSES) “RadioSun” international network aims to create a solid
  foundation for the successful exploitation of upcoming solar radio
  observational facilities, as well as intensive use of the existing
  observational tools, advanced theoretical modeling of relevant physical
  processes and observables, and training a new generation of solar
  radio physicists. The RadioSun network links research teams from China,
  Czech Republic, Poland, Russia and the UK. This mini-volume presents
  research papers based on invited reviews and contributed talks at
  the 1st RadioSun workshop in China. These papers cover a broad range
  of research topics and include recent observational and theoretical
  advances in solar radiophysics, MHD seismology of the solar corona,
  physics of solar flares, generation of radio emission, numerical
  modeling of MHD and plasma physics processes, charged-particle
  acceleration and novel instrumentation.

---------------------------------------------------------
Title: Dynamics of the hard X-ray, gamma-ray, and microwave emission
    of solar flares produced by the active region NOAA 0069 in August 2002
Authors: Bogomolov, A. V.; Kashapova, L. K.; Myagkova, I. N.; Tsap,
   Yu. T.
2014ARep...58..156B    Altcode:
  Regularities have been searched for in the dynamics of characteristics
  of flare solar radiation during the development of the active region
  NOAA 0069 in the interval of August 14-24, 2002. The SONG (Solar
  Neutrons and Gamma rays) instrument onboard the Russian CORONAS-F Solar
  Observatory recorded hard X-ray and gamma-ray radiation in nine of the
  30 flares of class above C5 in this active region within the indicated
  time interval. It was obtained that, in accordance with the development
  of the active region, the X- and gamma-ray flux tended to increase at
  the flare maxima while the hard X-ray spectral index tended to decrease;
  flares with a harder radiation spectrum occurred in the sunspot umbra,
  i.e., in the region with the strongest magnetic fields.

---------------------------------------------------------
Title: Analysis of time structure of the radio and HXR-emission
    of solar flares produced by AR0069 and their connection with
    characteristics of SEP events
Authors: Myagkova, Irina; Kashapova, Larisa; Miteva, Rositsa;
   Bogomolov, Andrew
2014cosp...40E2212M    Altcode:
  The results of the experimental investigation of solar energetic
  particles acceleration and propagation based on the study of delays
  between radio and X-rays emission of flares produced by the active
  region 0069 in August 2002 are present. Parameters of SXR and HXR photon
  spectrum as characteristics of acceleration processes were compared with
  SEP flux, their maximal energy and spectral index. Structure analysis
  of delays between microwave, meter and X-ray emission was carried
  out in order to study processes of accelerated at the Sun particle
  propagation and possible mechanisms of additional acceleration. It was
  obtained that during this series of flares more powerful SEP events
  with higher energies were observed in time flares with the minimal
  delay between microwave and HXR emission. The obtained results are
  discussed in respect to possible models of the SEP propagation.

---------------------------------------------------------
Title: On the Flat Gradual Phase of the 21 July 2013 Flare
Authors: Kashapova, Larisa; Sych, Robert; Zhdanov, Dmitrii;
   Tokhchukova, Susanna
2014cosp...40E1413K    Altcode:
  We present results of study of energy release process in the C3.1
  solar flare occurred on July 21, 2013. This event demonstrated about
  30-minutes duration flat period in the X-ray flux curve in the 3-12
  keV energy band during the gradual phase of the flare. Existence of
  this particular shape period was confirmed by EUV observations by
  EVE/SDO and microwave data. The reasons of such long suppression of
  plasma cooling are studied using the analysis of temporal profiles of
  EUV, X-ray, microwave emission and plasma parameters (temperature and
  emission measure). The aim of the study is the revealing and analysis
  of quasi-periodic pulsations which could be an indicator of the energy
  input or cooling suppressing during the studied period. Special
  attention is given to the analysis of microwave spectra obtained
  by RATAN-600 and Badary Broadband Microwave Spectropolarimeters
  (BBMS). The obtained results are discussed from the point of view of
  different mechanisms explaining the long duration events (LDE).

---------------------------------------------------------
Title: CORONAS-F detection of gamma-ray emission from the solar
    flare on 29 October 2003
Authors: Kurt, Victoria; Kashapova, Larisa; Yushkov, Boris; Kudela,
   Karel; Galkin, Vladimir
2014cosp...40E1705K    Altcode:
  Appreciable HXR/gamma-ray emissions in the 0.015-150 MeV energy
  range associated with the solar flare on 29 October 2003 (X10/3B) were
  observed at 20:41-20:58 with the SPR-N and SONG instruments onboard the
  CORONAS-F mission. Two time intervals were identified which showed major
  changes in the intensity of these emissions. To specify the details
  of the spectral changes with time, we fitted the SONG energy loss
  spectra with a three-component model of incident gamma-ray spectrum:
  (1) a power law in energy, assumed to be due to electron bremsstrahlung;
  (2) a broad continuum produced by nuclear de-excitation gamma-lines;
  and (3) a broad gamma-line generated from pion decay. We study the
  relationship between non-imaging observations, particularly between time
  of pion-decay emission onset and motions in this solar flare, using HXR
  foot points (FP) separation and flare shear temporal behavior presented
  by (Ji et al., 2008). In this work it was shown that significant
  FP converging and unshearing motion occurred during the first flare
  interval. During this interval the primary bremsstrahlung extended to
  tens of MeV and de-excitation gamma-lines dominated. During the second
  interval after 20:45 the FPs began to move apart. We found out that
  starting from 20:46, the gamma-emission spectrum revealed a feature
  attributed to pion-decay. It means that the effective acceleration of
  protons to energies above 300 MeV (pion-production threshold) occurred
  coincidently with a change of the flare magnetic structure. The maximum
  intensity of the pion-decay gamma emission was observed at 20:49 and
  proved to be 2.0•10-4 photons cm-2 s-1 MeV-1 at 100 MeV. This flare
  was accompanied by GLE-66. Using the data of the world neutron monitor
  network, we found its onset as 20:59 which corresponds to a reasonable
  propagation time of protons with ~ 0.5-2 GeV energy on the assumption
  that proton acceleration began at 20:46.

---------------------------------------------------------
Title: The subsecond pulses during the August 10, 2011 flare
    by observations of RATAN-600 and the 4-8 GHz Siberian solar
    spectropolarimeter
Authors: Kashapova, L. K.; Tokhchukova, S. Kh.; Zhdanov, D. A.; Bogod,
   V. M.; Rudenko, G. V.
2013Ge&Ae..53.1021K    Altcode:
  We present the results of a study of the subsecond pulses (SSPs)
  registered in the microwaves during the C2.4 solar flare. The event
  occurred on August 10, 2011, in the 11236 active region near the
  western limb and reached a maximum at 0935 UT. Subsecond pulses
  were registered by RATAN-600 for the first time when this flare
  reached its maximum. The fact of detection of SSPs was confirmed by
  simultaneous observations carried out with a spectropolarimeter at
  the Radio Astrophysical Observatory, Institute of Solar-Terrestrial
  Physics. A former analysis of the emission nature of the main flare
  source revealed the presence of a high-temperature ( T &gt; 30 MK)
  source that determined both the microwave and X-ray emission parameters
  of this event. We have compared the temporal variations of the SSPs
  microwave emission with the variations of the plasma parameters
  (temperature and emission measure) taken from observations with the
  FERMI space telescope with a subsecond time resolution. The obtained
  results suggest that the nature of SSP generation, as well as of the
  flare itself, was determined by the high-temperature source.

---------------------------------------------------------
Title: First results of radio observations of the sun and powerful
    discrete radio sources using the Irkutsk Radar
Authors: Vasil'ev, R. V.; Kushnarev, D. S.; Kashapova, L. K.; Lebedev,
   V. P.; Medvedev, A. V.; Nevedimov, N. I.; Ratovskii, K. G.
2013ARep...57..872V    Altcode:
  Using the Irkutsk Incoherent Scattering Radar, it is demonstrated that
  the high sensitivity of such radars, which are usually used for studies
  of the Earth's ionosphere, also enables their use in a passive mode for
  observations of astronomical radio sources. Observations of solar flares
  accompanied by coronal mass ejections and of quasi-stationary radio
  sources on the Sun have been carried out. In addition, scintillations of
  several of the brightest discrete radio sources (Cygnus A, Cassiopeia A,
  and the Crab Nebula) have been studied over several months. These data
  can also be useful for studies of the ionosphere and interplanetary
  space.

---------------------------------------------------------
Title: Coronal mass ejections in July 2005 and an unusual heliospheric
    event
Authors: Livshits, M. A.; Belov, A. V.; Shakhovskaya, A. I.; Eroshenko,
   E. A.; Osokin, A. R.; Kashapova, L. K.
2013CosRe..51..326L    Altcode:
  Using the events in July 2005 as an example, the causes and
  peculiarities of Forbush effects produced by solar sources remote
  from the central zone are discussed. The event in question differs
  from other effects observed at the periphery of interplanetary
  disturbances by strong variations in cosmic rays on the background
  of weak disturbances in the solar wind and magnetic field of the
  Earth. The cloud of magnetized plasma ejected from the Sun was large
  and fast, but it passed to the west from the Sun-Earth line. According
  to performed estimates, the mass of the ejected substance was close to
  the upper boundary of mass for coronal mass ejections (CMEs). Anomalous
  parameters and high modulation capability of the formed solar wind
  disturbance are explained, in particular, by the fact that it combined
  several CMEs and that the last fast disturbance was prepared by a series
  of impulsive events in the active region of the Sun. Usually, such a
  great mass is ejected directly after the main energy release in strong
  solar flares. In the given case, a powerful MHD disturbance occurred
  approximately half an hour after a maximum of hard X-ray burst under
  the conditions when gas pressure in the flare loops became close to
  magnetic pressure, which was just a premise of the largescale ejection.

---------------------------------------------------------
Title: Modeling of Hα Eruptive Events Observed at the Solar Limb
Authors: Kotrč, P.; Bárta, M.; Schwartz, P.; Kupryakov, Y. A.;
   Kashapova, L. K.; Karlický, M.
2013SoPh..284..447K    Altcode: 2012SoPh..tmp..290K; 2012SoPh..tmp..269K
  We present spectra and slit-jaw images of limb and on-disk eruptive
  events observed with a high temporal resolution by the Ondřejov
  Observatory optical spectrograph. Analysis of the time series of
  full width at half-maximum (FWHM) in Hα, Hβ, and radio and soft
  X-ray (SXR) fluxes indicates two phenomenologically distinct types
  of observations which differ significantly in the timing of FWHM
  and SXR/radio fluxes. We investigated one such unusual case of a
  limb eruptive event in more detail. Synthesis of all observed data
  supports the interpretation of the Hα broadening in the sense of
  regular macroscopic plasma motions, contrary to the traditional
  view (emission from warm dense plasma). The timing and observed
  characteristics indicate that we may have actually observed the
  initiation of a prominence eruption. We test this scenario via modeling
  of the initial phase of the flux rope eruption in a magnetohydrodynamic
  (MHD) simulation, calculating subsequently - under some simplifying
  assumptions - the modeled Hα emission and spectrum. The modeled and
  observed data correspond well. Nevertheless, the following question
  arises: To what extent is the resulting emission sensitive to the
  underlying model of plasma dynamics? To address this issue, we have
  computed a grid of kinematic models with various arbitrary plasma
  flow patterns and then calculated their resulting emission. Finally,
  we suggest a diagnostics based on the model and demonstrate that it
  can be used to estimate the Alfvén velocity and plasma beta in the
  prominence, which are otherwise hard to obtain.

---------------------------------------------------------
Title: Microwave Quasi-periodic Radio Pulsations in the 2012 March
    08 Solar Flare
Authors: Zhdanov, D. A.; Kashapova, L. K.; Altyntsev, A. T.; Myshyakov,
   I. I.; Zandanov, V. V.
2013CEAB...37..563Z    Altcode:
  We describe microwave observations of quasi-periodic pulsations
  from the C6.8 flare on 2012 March 08. The radio observations were
  made by the Siberian Solar Radio Telescope and Siberian Solar Radio
  Spectropolarimeter. The microwave quasi-periodic pulsations were
  accompanied by hard X-ray emissions which were obtained by the Fermi
  Gamma-ray Space Telescope. We considered both magnetohydrodynamic
  oscillations and injection of accelerated electrons as the possible
  cause of microwave pulsations.

---------------------------------------------------------
Title: On the Possible Mechanisms of Energy Release in a C-class Flare
Authors: Kashapova, L. K.; Tokhchukova, S. K.; Rudenko, G. V.; Bogod,
   V. M.; Muratov, A. A.
2013CEAB...37..573K    Altcode:
  We present the study of the C2.4 flare which occurred at 9:35 UT, 2011
  August 10 in the AR 11263 near the western limb. It was observed by
  RATAN-600 and the Siberian Solar Radio Spectropolarimeter in microwaves
  (MW) and by RHESSI and FERMI in hard X-rays (HXR). A peculiarity of
  this event was the detection of HXR flux with energies above 25 keV
  that is not typical for such weak flares. The good correlation between
  HXR and MW time profiles indicates the generation of both HXR and MW
  emission by a common population of electrons. Results of fitting the
  HXR spectra revealed that the flare emission of energies above 25 keV
  could be generated both by non-thermal electrons and a high-temperature
  source (T&gt; 30 MK). We reconstructed the microwave spectra using the
  GX_Simulator code for 3D modeling of gyrosynchrotron microwave emission
  (Fleischmann et al., 2011) . The input flare plasma parameters were
  obtained from HXR spectra and the magnetic field structure was obtained
  by extrapolation of the photospheric magnetic field from HMI/SDO. The
  results were compared with existing theoretical models and observations
  of other authors.

---------------------------------------------------------
Title: On a Signature of a Flux-rope Formation by Vortex Motions in
    its Footpoint
Authors: Kotrč, P.; Bárta, M.; Kupryakov, Yu. A.; Kashapova, L. K.
2013CEAB...37..513K    Altcode:
  We analyzed Hα spectrograms and slit-jaw filtergrams of active regions
  NOAA 10311 and 10314 observed by the Ondřejov flare spectrograph near
  the western limb on March 19, 2003. Several pre-flares and medium
  flares C, M, X (according to GOES classification) occurred in this
  active region during our period of observation. We observed a process
  of intensive creation of an active region filament. Then the filament
  changed its contrast in relation to the surrounding chromosphere. From
  details observed in the filtergrams and spectra we conclude that during
  this process the filament/flux-rope was twisted by vortex motions in
  its footpoint. The energy accumulated gradually in the configuration of
  magnetic field was then released during a series of flares. We discuss
  the observed phenomena and try to explain them in frame of generally
  accepted models of physical processes in solar flares.

---------------------------------------------------------
Title: On a Flat-shape Emission in the Solar Flare on 7th June 2012
Authors: Kotrč, P.; Kupryakov, Yu. A.; Kashapova, L. K.; Bárta, M.
2013CEAB...37..555K    Altcode:
  We present results of the study of the C1.5 solar
  flare~(SOL2012-06-07T05:56) which occurred on June 7, 2012. This weak
  flare showed an extraordinary long flat emission in the X-ray flux curve
  in the 3-12 keV energy band. Duration of this flat period was about 10
  minutes while the duration of the flare was almost 20 minutes. As this
  particular shape was observed both by RHESSI and FERMI, it could not
  be caused by an instrumental effect. We analyzed the optical spectra
  and slit-jaw images from the solar spectrograph in Ondřejov and in
  the hard X-ray by RHESSI as well as EUV data obtained by SDO and all
  available microwave data. We found that the "flat emission" period was
  also observed in microwaves (5-17 GHz). During this period the motion
  of the flare source from the spot to south direction was revealed. A
  localized maximum of the chromospheric emission was also shifting in the
  same direction. Quasi-periodic pulsations with <P />periods of about
  5 minutes were detected in evolution of the electron temperature that
  is an evidence of the energy input during the "flat emission" period.

---------------------------------------------------------
Title: Relationship between nonthermal and gasdynamic processes in
    powerful solar flares
Authors: Livshits, M. A.; Kashapova, L. K.
2012Ge&Ae..52..892L    Altcode:
  The relationship between gas-dynamic processes and particle acceleration
  is illustrated using three examples. For the flare of July 6, 2006,
  observations show that explosive evaporation of the chromosphere occurs
  in the pulse phase. In addition, the coronal mass emission (CME) related
  to this flare reflects the primary energy release. In the strong limb
  flare of July 14, 2005, the CME observed in the external layers of the
  corona seems to be a consequence of repeated energy releases and plasma
  emissions. Apparently, this is indicated by the additional emission
  in the decimeter range, which is typical of posteruptive processes. An
  example of a weak flare during the decay phase of the strong event of
  April 15, 2001, was also accompanied by a decimeter burst.

---------------------------------------------------------
Title: Magnetic field dynamics based on SOHO/MDI data in the region
    of flares related to halo coronal mass ejections
Authors: Fainshtein, V. G.; Popova, T. E.; Kashapova, L. K.
2012Ge&Ae..52.1075F    Altcode:
  Variations in the photospheric magnetic field in the region of
  solar flares, related to halo coronal mass ejections (HCMEs) with
  velocities V &gt; 1500, 1000 &lt; V &lt; 1500, and V &lt; 650 km/s,
  have been studied based on SOHO/MDI data. Using data with a time
  resolution of 96 min, it has been indicated that on average the &lt;
  B <SUB>L</SUB>&gt; and &lt;| B <SUB>L</SUB>|&gt; field characteristics
  increase nonmonotonically during 1-1.5 days before a flare and decrease
  during 0.5-1 days after a flare for groups of ejections with V &gt;
  1000 km/s for all considered HCME groups. Angle brackets designate
  averaging of the measured B <SUB>L</SUB> magnetic field component and
  its magnitude | B <SUB>L</SUB>| within an area with specified dimensions
  and the center coincident with the projection onto the region where the
  flare center field is measured. It has been established that a solar
  flare related to an HCME originates when the &lt; B <SUB>L</SUB>&gt;
  and &lt;| B <SUB>L</SUB>|&gt; values are larger than the boundary
  values in the flare region. Based on 1-min data, it has been found
  for several HCMEs with V &gt; 1500 km/s that the beginning of powerful
  flares related to ejections is accompanied by rapid impulsive or stepped
  variations in &lt; B <SUB>L</SUB>&gt; and &lt;| B <SUB>L</SUB>|&gt;
  near the center of a flare with a size of approximately 4.5°. It has
  been established that the HCME velocity positively correlates with
  the |&lt; B <SUB>L</SUB>&gt;| value at the flare onset.

---------------------------------------------------------
Title: Detection of Acceleration Processes During the Initial Phase
    of the 12 June 2010 Flare
Authors: Kashapova, L. K.; Meshalkina, N. S.; Kisil, M. S.
2012SoPh..280..525K    Altcode: 2012SoPh..tmp..189K; 2012arXiv1207.5896K
  We present an analysis of the plasma parameters during the initial
  phase of the 12 June 2010 flare (SOL2010-06-12T00:57). A peculiarity
  of the flare was the detection of γ-ray emission that is unusual for
  such weak and short event. The analysis revealed the presence of a
  flare precursor detected about five minutes before the flare onset
  in 94 Å images which spatially coincided with the non-polarized
  microwave (MW) source at 17 GHz (the Nobeyama Radio Heliograph)
  that is the Neutral Line associated Source (NLS). A comparison of the
  results obtained from MW data by the Nobeyama Radio Polarimeters and
  the multi-frequency Siberian Radioheliograph (the new 10-antenna
  radio heliograph prototype at 4.6 and 6.4 GHz) and hard X-ray
  (HXR) observations by the Fermi Gamma-ray Space Telescope reveal the
  presence of accelerated electrons during the flare's initial phase. The
  analysis of MW and HXR spectra also confirms the presence of accelerated
  particles. Moreover, a good temporal correlation between several light
  curves in different HXR energy bands and at MW frequencies indicates
  the generation of both HXR and MW emission by a common population of
  accelerated electrons. Detection of accelerated particles during the
  initial phase of the flare and soft-hard-harder (SHH) behavior of the
  spectra indicate several episodes of particle acceleration and confirm
  the non-impulsive type of the flare evolution.

---------------------------------------------------------
Title: Observation of the powerful solar flare of October 27, 2002
    on the far side of the sun
Authors: Vybornov, V. I.; Livshits, M. A.; Kashapova, L. K.;
   Mitrofanov, I. G.; Golovin, D. V.; Kozyrev, A. S.; Litvak, M. L.;
   Sanin, A. B.; Tret'yakov, V. I.; Boynton, W.; Shinohara, K.; Hamara, D.
2012ARep...56..805V    Altcode: 2012AZh....89..888V
  Observations of the hard X-ray and radio event of October 27, 2002
  are analyzed. This flare was observed from near-Martian orbit by
  the HEND instrument developed at the Space Research Institute of
  the Russian Academy of Sciences and installed on the Mars Odyssey
  satellite. Although this powerful flare was observed far over the
  eastern solar limb, the extended source associated with the flare
  was detected by RHESSI at energies up to about 60 keV. The eruptive
  event was observed in the radio at the Nobeyama Radio Observatory. The
  properties of the X-ray radiation are used to calculate the spectrum
  of the accelerated electrons responsible for the observed radiation,
  assuming that the target is thick for a Martian observer and thin for
  a terrestrial observer. The results are compared with the results of
  radio observations. The conditions for electron propagation in the
  corona are discussed.

---------------------------------------------------------
Title: On Detection of Balmer-Series Lines Response to Accelerated
    Particles in Solar Flares
Authors: Kotrč, P.; Kashapova, L. K.; Kupryakov, Y. A.
2012ASPC..454..337K    Altcode:
  Comparison of the Balmer series lines with HXR and microwave emissions
  are used as tools for study of the chromospheric response to effects
  of accelerated particle beams in solar flares. We studied the Hα
  and Hβ lines and the ratio of the line profiles for several solar
  flares observed with a high cadence to find and to analyze variations
  predicted from the theoretical simulations of Kašparová &amp; Heinzel
  (2002). The profiles extracted at individual kernels during different
  flare phases were analyzed with respect to the radio and X-ray data
  patterns. We found that the theoretical predictions of the Hα/Hβ
  line profile ratios and the observations were in a good qualitative
  agreement. However, as concerns quantitative correspondence, we found
  some difference in position of the predicted profile ratio maxima,
  moment of arising and the duration of the effect, influence of energy
  cutoff of electron beam. We try to find some explanations for those
  discrepancies and discuss perspectives of simultaneous observations
  of Balmer series lines.

---------------------------------------------------------
Title: Particle transport effects in solar flares for interpretation
of HXR and MW emission: theory versus observations
Authors: Zharkova, V. V.; Taras, S.; Kashapova, L.; Kuznetsov, A.
2011AGUFMSH41A1893Z    Altcode:
  In this paper we discuss the effects of different energy loss mechanisms
  on resulting hard X-ray and MW emission of beam electrons injected in
  the loop top in the corona and precipitating into loop footpoints. For
  this purpose we use numeric solutions of Fokker-Planck equation
  considering collisional and Ohmic energy losses and anisotropic
  scattering in converging magnetic field for different scenarios
  of particle injections with respect to pitch angle anisotropy and
  different flaring atmosphere models. Electron beam distributions
  obtained in collisional, collisional plus Ohmic losses, collisional
  plus Ohmic plus turbulent losses for the models with different magnetic
  convergence factors are compared. The resulting HXR and MW emission
  and polarisation for each models are compared and implications for
  the interpretation of observations are also discussed.

---------------------------------------------------------
Title: Effect of a self-induced electric field on the electron beam
    kinetics and resulting hard X-ray and microwave emissions in flares
Authors: Zharkova, V. V.; Meshalkina, N. S.; Kashapova, L. K.;
   Altyntsev, A. T.; Kuznetsov, A. A.
2011Ge&Ae..51.1029Z    Altcode:
  The kinetics of beam electron precipitation from the top of a loop
  into the solar atmosphere with density gradients and an increasing
  magnetic field have been generally described. The Fokker-Planck
  equations are solved with regard to Coulomb collisions and the effect
  of the electric field induced by this beam. The photon spectra and
  polarization degree in hard X-ray (10-300 keV) and microwave (1-80
  GHz) emissions are simulated under different assumptions regarding
  the beam electron distribution function. The simulation results are
  compared with the flare observations on March 10, 2001, and July 23,
  2002, visible at different position angles. It has been indicated that
  the coincidence of the theoretical photon spectra with simultaneous
  observations of the hard X-ray and microwave emissions of these flares
  is the best for models that not only take into account collisions,
  but also the electric field induced by electron fluxes propagating in
  flare loops with very weakly or moderately converging magnetic fields.

---------------------------------------------------------
Title: Physics of post-eruptive solar arcades: Interpretation of
    RATAN-600 and STEREO spacecraft observations
Authors: Livshits, M. A.; Urnov, A. M.; Goryaev, F. F.; Kashapova,
   L. K.; Grigor'eva, I. Yu.; Kal'Tman, T. I.
2011ARep...55..918L    Altcode: 2011AZh....88..997L
  Results of simultaneous measurements of radiation fluxes from
  post-eruption arcades on the Sun at 171, 195, 284, and 304 Å (from
  STEREO spacecraft data) and at radio wavelengths (from the RATAN-600
  radio telescope) are presented. An original probabilistic approach
  developed earlier by Urnov was used to determine the differential
  emission measure. This method requires no regularization, and the
  obtained results do not depend on the choice of the temperature
  grid. This approach has yielded the differential measure of emission at
  temperatures approximately from 0.3 to 15 MK. The subsequent calculation
  of thermal magnetobremsstrahlung in a multi-temperature model with
  the magnetic field decreasing with height produces a spectrum similar
  to that observed on RATAN-600. Thus, in many non-stationary events
  with modest powers, a thermal multi-temperature model is quite able
  to explain the emission of post-eruption arcade systems, and it is not
  necessary to invoke the emission of accelerated particles. The proposed
  model enables direct estimation of the ratio of the magnetic and gas
  pressures at the tops of post-eruption arcades, and determination
  of the conditions required for the origin of secondary nonstationary
  processes in the decay stage of the main flare.

---------------------------------------------------------
Title: Erratum to: "Culmination of the flare activity of group 10786
in July 2005: X-ray observations from near-Mars and near-Earth orbits"
Authors: Livshits, M. A.; Golovin, D. V.; Kashapova, L. K.; Mitrofanov,
   I. G.; Kozyrev, A. S.; Litvak, M. L.; Sanin, A. B.; Tret'yakov, V. I.;
   Boynton, W.; Shinohara, K.; Hamara, D.
2011ARep...55..943L    Altcode:
  No abstract at ADS

---------------------------------------------------------
Title: Diagnostics of electron beam properties from the simultaneous
    hard X-ray and microwave emission in the 2001 March 10 flare
Authors: Zharkova, V. V.; Meshalkina, N. S.; Kashapova, L. K.;
   Kuznetsov, A. A.; Altyntsev, A. T.
2011A&A...532A..17Z    Altcode: 2011arXiv1105.3508Z; 2010A&A...532A..17Z
  Context. Microwave (MW) and hard X-ray (HXR) data are thought to be
  powerful means of investigating the mechanisms of particle acceleration
  and precipitation in solar flares, reflecting different aspects
  of electron interaction with ambient particles in the presence of a
  magnetic field. Simultaneous simulation of HXR and MW emission with the
  same populations of electrons is still a big challenge for interpreting
  observations of real events. Recent progress in simulations of particle
  kinetics with the time-dependent Fokker-Planck (FP) approach offers an
  opportunity to produce this interpretation. <BR /> Aims: In this paper
  we apply the FP kinetic model of precipitation of electron beam with
  energy range from 12 keV to 1.2 MeV to the interpretation of X-ray and
  MW emissions observed in the flare of 2001 March 10. <BR /> Methods:
  The theoretical HXR and MW emissions were calculated by using the
  distribution functions of electron beams found by solving time-dependent
  approach in a converging magnetic field for anisotropic scattering
  of beam electrons on the ambient particles in Coloumb collisions and
  Ohmic losses. <BR /> Results: The simultaneously observed HXR photon
  spectra and frequency distribution of MW emission and polarization
  were fit by those simulated from FP models that include the effects
  of electric field induced by beam electrons and precipitation onto a
  converging magnetic loop. Magnetic field strengths in the footpoints on
  the photosphere were updated with newly calibrated SOHO/MDI data. The
  observed HXR energy spectrum above 10 keV is shown to be a double power
  law that was precisely fit by the photon HXR spectrum simulated for the
  model including the self-induced electric field but without magnetic
  convergence. The MW emission simulated for different models of electron
  precipitation revealed a better fit (above 90% confidence level) to the
  observed distribution at higher frequencies for the models combining
  collisions and electric field effects with a moderate magnetic field
  convergence of two. The MW simulations were able to reproduce closely
  the main features of the MW emission observed at higher frequencies:
  the spectral index, the frequency of peak intensity and the frequency of
  the MW polarization reversal, while at lower frequencies the simulated
  MW intensities are lower than the observed ones.

---------------------------------------------------------
Title: Culmination of the flare activity of Group 10786 in July 2005:
    X-Ray observations from near-mars and near-earth orbits
Authors: Livshits, M. A.; Golovin, D. V.; Kashapova, L. K.; Mitrofanov,
   I. G.; Kozyrev, A. S.; Litvak, M. L.; Sanin, A. B.; Tret'yakov, V. I.;
   Boynton, W.; Shinohara, K.; Hamara, D.
2011ARep...55..551L    Altcode: 2011AZh....88..598L
  A detailed study of two major solar flares that occurred in Group
  10786 at the time of its disappearance behind the western limb
  is presented. The flares of July 14, 2005 were previously studied
  fairly poorly, as no RHESSI hard X-ray observations were available
  for themaxima of the twomost powerful of these flares. Observations
  carried out using the HEND equipment (on the Mars Odyssey spacecraft)
  developed at the Institute for Space Research in Moscow are used
  here to fill this gap. In the first flare, an intense, impulsive
  burst occurred at 07:23 UT, about 1.5 h after the onset of a weak,
  prolonged event. While processes in the neighborhood of the northern
  spot dominated in the flares of July 5-9, a powerful impulsive energy
  release on July 14 emerged when the flare process that originated
  in the North reached the southern spot. Our analysis of the flare
  activity of this medium-sized group reveals a gradual enhancement of
  the flare activity and a strong interaction between the acceleration
  above the magnetic-field neutral line and in the immediate vicinity
  of the spots. At the time of the culmination of the flare activity in
  the group on July 13 and 14, the pattern of nonstationary processes
  changes: fast coronal mass ejections form after a series of impulsive
  energy-release events. Spacecraft observations of the burst of July
  14 after 11 UT at points separated in longitude (on RHESSI and Mars
  Odyssey) revealed clear anisotropy of the flare emission at energies
  exceeding 80 keV.

---------------------------------------------------------
Title: The effect of energetic particle beams on the chromospheric
    emission of the 2004 July 25 flare
Authors: Zharkova, V. V.; Kashapova, L. K.; Chornogor, S. N.;
   Andrienko, O. V.
2011MNRAS.411.1562Z    Altcode:
  In this paper the role of particle beams in the generation of a
  close spatial and temporal correlation between hard X-ray (HXR)
  energy and Hα line emission bursts in the solar flare of 2004 July
  25 is discussed. The light curves in the HXR emission and Hα line
  reveal that the pre-flare and main flare events are correlated with the
  variations of line-of-sight (LOS) magnetic flux. The HXR emission shows
  three main bursts during the main flare phase, which are accompanied by
  Hα intensity increases. The latter appear in 10 locations (kernels) at
  different times in succession; the kernel locations are associated with
  strong magnetic sources situated on the opposite side from the magnetic
  neutral line (MNL). The appearance of Hα kernels in the pre-flare
  event and those at the start of the main event ia correlated very
  closely (within a few seconds) with the HXR emission observed by the
  Reuven Ramaty High-Energy Solar Spectroscopic Imager (RHESSI) (HXR+Hα
  kernels), while the appearance of some others, not associated with HXR
  emission, was delayed by tens of seconds. Electron-beam parameters were
  derived from the RHESSI spectra in which the observed HXR photon flux
  was corrected for the self-induced electric field effect. Possible
  implications of this electric field on the production of transient
  magnetic fields observed during the flare are discussed. The Hα
  emission observed during the first burst was simulated in a hydrodynamic
  atmosphere for 5 levels plus a continuum hydrogen atom with the full
  non-local thermodynamic equilibrium (non-LTE) approach combining
  radiative, thermal and non-thermal excitation and ionization by an
  electron beam with the derived parameters. The simulated temporal
  profiles of Hα emission produced by non-thermal hydrogen excitation
  revealed a very good fit to the observed ones in the HXR+Hα kernels
  and 10-20 s delays in the other kernels. This allows us to speculate
  that Hα emission is caused mainly by electrons in the HXR+Hα kernels
  and mainly by protons in the others.

---------------------------------------------------------
Title: On the Chromospheric Response At The Pre-CME Phase Of The 18
    March 2003 Solar Flare
Authors: Kashapova, L. K.; Kotrč, P.; Kupryakov, Yu. A.
2011CEAB...35..125K    Altcode:
  We present a study of the X1.5 solar flare that occurred in the AR
  10314 and was followed by a partial halo CME. Our main target was
  to find characteristic parameters associated with the pre-CME and
  CME phase. Special attention is devoted to parameters obtained from
  chromospheric observations. We analysed Hα spectra and Hα slit-jaw
  images from the Ondřejov Multichannel Flare Spectrograph observed with
  a high temporal resolution. Comparison of the Hα shift and the HXR
  data revealed that before the CME onset each injection of accelerated
  particles to the chromosphere was followed by upward mass motions with
  a delay of about 45 seconds. We did not find a significant value of the
  Hα shift that could be associated with Moreton wave velocities during
  the ejection phase. All values of the Hα blue shift corresponded to
  the evaporation process. Thus the role of the chromosphere in the CME
  preparatory phase was to increase the amount of the mass above the
  flare region which was then released by the CME.

---------------------------------------------------------
Title: Study of energy release and transport processes of the 14th
    July 2005 flares in AR~10786
Authors: Sizykh, T. S.; Kashapova, L. K.
2011CEAB...35...93S    Altcode:
  We studied acceleration processes in two large flares (M1.0 and X1.2)
  that originated in the active region 10786 on 14 July 2005 when the
  region was partially occulted at the west limb of the Sun. The M1.0
  flare had a thermal spectrum while the X1.2 flare had a significant
  non-thermal component. A comparison of temperature (T) vs. emission
  measure (EM) diagrams and spectral index vs. flux diagrams for the
  X1.2 flare shows that the impulsive phase corresponded to the period of
  rising T and EM. The T vs. EM diagrams of both flares had small turns,
  near the time of flare impulsive phase, which could be associated with
  CME events.

---------------------------------------------------------
Title: The post-eruptive arcade formation in the limb event on July
    31, 2004 from microwave solar observations with the RATAN-600 radio
    telescope
Authors: Grigoryeva, I. Yu.; Kashapova, L. K.; Borovik, V. N.;
   Livshits, M. A.
2010SunGe...5...58G    Altcode:
  A CME/flare event occurred at the western limb on 31 July 2004. Five
  successive multi-wavelength scans in centimeter range were obtained
  with the RATAN-600 radio telescope starting at the early stage of
  post-eruptive arcade formation (24 min after a C8.3 flare peak)
  and lasting for 4 hours. Microwave radio emission of the arcade was
  rather intense at initial stage indicating a predominant contribution
  of thermal emission and then considerably decreased during the decay
  phase. Its maximum was co-spatial with the 195 Å Fe XII loop tops. At
  the end of microwave observations the contribution of the emission from
  accelerated particles became significant. The similarity of microwave
  characteristics of two eruptive events (on 31 July 2004 at the western
  limb and on 25 January 2007 at the eastern limb) is shown.

---------------------------------------------------------
Title: Catalogue of solar flare spectra observed at Ondrejov in
    1998-2007
Authors: Kupryakov, Yu. A.; Kotrc, P.; Kashapova, L. K.
2010SunGe...5...61K    Altcode:
  We present a catalogue of solar flare data observed with two Ondřejov
  optical spectrographs during 1998-2007 years. This database was
  created to enable the data processing more convenient for users
  interested in the study of the energy release and transport in solar
  flares. The spectra and Hα filtergrams were obtained both at the
  Multichannel Flare Spectrograph (MFS) and at the Large Horizontal
  Spectrograph (HSFA2). The catalogue contains basic information
  about time of observation of solar flares, their location in
  AR, importance, availability of related data at the selected
  X-ray, EUV and radio instruments. The catalogue is available at
  www.asu.cas.cz/~sos/flare_archive.html.

---------------------------------------------------------
Title: Latitudinal and Solar-Cycle Variations of the White-Light
    Corona from SOHO/LASCO Observations
Authors: Fainshtein, V. G.; Tsivileva, D. M.; Kashapova, L. K.
2010SoPh..267..203F    Altcode: 2010SoPh..tmp..182F
  SOHO/LASCO data were used to obtain the latitudinal and radial
  distributions of the brightness of the K- and F-corona in the period
  of 1996 - 2007, and their solar-cycle variations were studied. Then
  an inversion method was employed to obtain the radial distributions
  of the electron density N<SUB>e</SUB>(R,θ) for various latitude
  values on the coronal images. Our values of N<SUB>e</SUB>(R,θ) are
  in good agreement with the findings of other authors. We found that
  in an edge-on streamer belt the electron density, like the K-corona
  brightness, varies with distance more slowly in the near-equatorial rays
  than in near-polar regions. We have developed a method for assessing
  the maximum values of the electron density at the center of the face-on
  streamer belt in its bright rays and depressions between them. Not
  all bright rays observed in the face-on streamer belt are found to be
  associated with an increased electron density in them. Mechanisms for
  forming such rays have been suggested.

---------------------------------------------------------
Title: Properties of the magnetic fields of coronal holes with
    active regions
Authors: Fainshtein, V. G.; Stepanian, N. N.; Rudenko, G. V.;
   Malashchuk, V. M.; Kashapova, L. K.
2010BCrAO.106....1F    Altcode:
  We determine the structure of the magnetic fields of coronal holes (CHs)
  and investigate its change in connection with the emergence of active
  regions (ARs) in CHs. Based on our observations in the HeI 1083 nm line
  performed with the CrAO TST-2 telescope, we have selected CHs of two
  types: without (15 CHs) and with (28 CHs) ARs. Magnetograms obtained at
  the Kitt Peak National Solar Observatory have been used to calculate the
  magnetic fields of the same objects. We have calculated magnetic field
  characteristics by Rudenko’s method in the potential approximation at
  several heights in the corona, namely, the average (over the CH area)
  radial field component &lt; B <SUB> r </SUB>&gt; and its magnitude &lt;|
  B <SUB> r </SUB>|/ B&gt; and the maximum and minimum (over the CH area)
  values of B <SUB> r </SUB>. The distributions of the isolines of these
  parameters superimposed on the CH images and the field lines of the
  calculated magnetic field have been constructed with resolutions of
  33.4″ and 100.2″ on the solar surface. Analysis of these data has
  yielded the following results: <P />The field lines originating in
  CHs without ARs are open or very high loops that are closed outside
  CHs. The latter occurs in completely or partially closed CHs.

---------------------------------------------------------
Title: Determination of Geometric and Kinematical Parameters of
    Coronal Mass Ejections Using STEREO Data
Authors: Fainshtein, V. G.; Tsivileva, D. M.; Kashapova, L. K.
2010AIPC.1216..416F    Altcode:
  We present a new, relatively simple and fast method to determine true
  geometric and kinematical CME parameters from simultaneous STEREO A,
  B observations of CMEs. These parameters are the three-dimensional
  direction of CME propagation, velocity and acceleration of CME front,
  CME angular sizes and front position depending on time. The method
  is based on the assumption that CME shape may be described by a
  modification of so-called ice-cream cone models. The method has been
  tested for several CMEs.

---------------------------------------------------------
Title: Investigation of acceleration processes of the 14th july 2005
    flare series occurred in ar 10786
Authors: Sizykh, Tatyana; Kashapova, Larisa
2010cosp...38.1975S    Altcode: 2010cosp.meet.1975S
  We present the results of acceleration process study in the flare
  series occurred 14th July 2005 on the western limb of the Sun. Our
  investigation is based on HXR data obtained by RHESSI. It was observed
  increasing of solar flare activity with X1.2 class flare at its
  culmination. The presence of accelerated electrons (the power-law
  component of HXR spectrum for energies more than 25 keV) was clearly
  signified only in the first (C3.8) and the last of studied flares. We
  applied lgT-1/2lgEM diagrams ( Jakimiec et al,1986) for quantitative
  study of HXR spectrums for all flares. For analysis of the flares
  showed presence of significant flux of accelerated electrons we also
  used diagrams made on base of parameters obtained from non-thermal
  part of the spectrum (flux, spectral index, spectral curvature, Grigis
  Benz 2009). The possible scenario of evolution of this active region
  is discussed.

---------------------------------------------------------
Title: Directivity of HXR Solar Flare Emission Obtained from
    Stereoscopic Observations by Mars Odyssey (HEND), RHESSI and CORONAS-F
    (SONG)
Authors: Livshits, Moisey; Golovin, Dmitry; Mitrofanov, Igor; Kozyrev,
   S. Alexander; Litvak, Maxim; Tretyakov, Vladislav; Sanin, Anton;
   Boynton, William V.; Kashapova, Larisa; Myagkova, Irina; Bogomolov,
   Andrey
2010cosp...38.2984L    Altcode: 2010cosp.meet.2984L
  Two powerful X-Ray flares were observed on 2005, July 14 by three
  spacecrafts whose heliolon-gitudes were spaced on 39 degrees. The flares
  were observed, as projected on the solar disc by Mars Odyssey (HEND)
  and seeing almost directly on the limb by RHESSI and CORONAS-F. The most
  intensive hard X-ray and gamma-ray flare (up to 2 MeV) was observed by
  HEND and SONG on 07:23 UT, and measured time profiles were similar,
  but the spectra were quite rather different. Particular pulses of
  flares were studied by data from different instruments with dif-ferent
  heliolongitudes, and conclusion was drawn that difference between fluxes
  at these flares is more likely due to a directivity of radiation. The
  emission directivity was more clearly seen for the source at the top
  of flare loop for burst observed near 11:00 UT.

---------------------------------------------------------
Title: Diagnostics of the beam anisotropy from the HXR and MW emission
    data in the flare of 10 March 2001.
Authors: Meshalkina, Natalia; Zharkova, Valentina; Kashapova, Larisa;
   Altyntsev, Alexander; Kuznetsov, Alexey
2010cosp...38.1963M    Altcode: 2010cosp.meet.1963M
  Microwave and hard X-ray data are thought to be powerful mean
  for investigating the mech-anisms of particle acceleration and
  precipitation in solar flares. In this paper X-ray and mi-crowave
  emission is investigated for the flare of 10 March 2010 previously
  studied by Altyntsev et al. (2008), who concluded there was a beamlike
  anisotropy in the particle distribution in the event. The simulations
  of HXR and MW emissions produced by beam electrons with en-ergies from
  12keV to 1.2 MeV are carried out by taking into account anisotropic
  scattering in converging magnetic field of beam electrons in Coloumb
  collisions and Ohmic losses by using time-dependent Fokker-Planck
  approach (Zharkova at al, AA, 2010; Kuznetsov and Zharkova, AA,
  2010). The simulated HXR photons spectra, MW emission spectra (1-80
  GHz) and polar-ization are compared with the observed ones using
  the magnetic field values updated with new calibrated MDI. Similar
  to the previous simulations (Altyntsev et al, 2008), we conclude the
  absence of a detectable magnetic field convergence in both HXR and MW
  emission. However, the simulated HXR photon spectra, MW emission and
  polarization reveal the best fit for the models including the effect
  of electric field induced by beam electrons show the both emission
  emitted from a slightly tilted loop in the flare location and not in
  the perpendicular direction deduced in earlier simulations.

---------------------------------------------------------
Title: Some properties of the continuous latitude distributions of
    the brightness of the K and F coronas as deduced from the LASCO data
Authors: Fainshtein, V. G.; Kashapova, L. K.; Tsivileva, D. M.
2009Ge&Ae..49.1106F    Altcode:
  Using two new methods for separating the K and F coronas and the LASCO
  C2 and C3 coronagraph data, continuous latitude distributions of the
  brightness of the K and F coronas have been obtained and examined as
  a function of the distance for different solar activity phases.

---------------------------------------------------------
Title: High-Energy Emission from a Solar Flare in Hard X-rays and
    Microwaves
Authors: Kundu, M. R.; Grechnev, V. V.; White, S. M.; Schmahl, E. J.;
   Meshalkina, N. S.; Kashapova, L. K.
2009SoPh..260..135K    Altcode: 2009arXiv0908.0385K
  We investigate accelerated electron energy spectra for different sources
  in a large flare using simultaneous observations obtained with two
  instruments, the Nobeyama Radio Heliograph (NoRH) at 17 and 34 GHz,
  and the Reuven Ramaty High Energy Solar Spectroscopic Imager (RHESSI)
  at hard X-rays. This flare is one of the few in which emission up to
  energies exceeding 200 keV can be imaged in hard X-rays. Furthermore,
  we can investigate the spectra of individual sources up to this
  energy. We discuss and compare the HXR and microwave spectra and
  morphology. Although the event overall appears to correspond to the
  standard scenario with magnetic reconnection under an eruptive filament,
  several of its features do not seem to be consistent with popular flare
  models. In particular we find that (1) microwave emissions might be
  optically thick at high frequencies despite a low peak frequency in
  the total flux radio spectrum, presumably due to the inhomogeneity
  of the emitting source; (2) magnetic fields in high-frequency radio
  sources might be stronger than sometimes assumed; (3) sources spread
  over a very large volume can show matching evolution in their hard
  X-ray spectra that may provide a challenge to acceleration models. Our
  results emphasize the importance of studies of sunspot-associated flares
  and total flux measurements of radio bursts in the millimeter range.

---------------------------------------------------------
Title: Eruptions of Magnetic Ropes in Two Homologous Solar Events
of 2002 June 1 and 2: a Key to Understanding an Enigmatic Flare
Authors: Meshalkina, Nataliya S.; Uralov, Arkadiy M.; Grechnev,
   Victor V.; Altyntsev, Alexander T.; Kashapova, Larisa K.
2009PASJ...61..791M    Altcode: 2009arXiv0908.0384M
  The goal of this paper is to understand the drivers, configurations,
  and scenarios of two similar eruptive events, which occurred in
  the same solar active region 9973 on 2002 June 1 and 2. The June 2
  event was previously studied by Sui, Holman, and Dennis (2006, ApJ,
  646, 605; 2008, Adv. Space Res., 41, 976), who concluded that it was
  challenging for popular flare models. Using multi-spectral data, we
  analyzed a combination of the two events. Each of the events exhibited
  an evolving cusp-like feature. We have revealed that these apparent
  “cusps” were most likely mimicked by twisted magnetic flux ropes,
  but unlikely to be related to the inverted Y-like magnetic configuration
  in the standard flare model. The ropes originated inside a funnel-like
  magnetic domain whose base was bounded by an EUV ring structure, and
  the top was associated with a coronal null point. The ropes appear to
  be the major drivers for the events, but their rise was not triggered
  by reconnection in the coronal null point. We propose a scenario and
  a three-dimensional scheme for these events in which the filament
  eruptions and flares were caused by interaction of the ropes.

---------------------------------------------------------
Title: High-Energy Emission from a Solar Flare in Hard X-Rays and
    Microwaves
Authors: Kundu, Mukul R.; Grechnev, V. V.; White, S. M.; Schmahl,
   E. J.; Meshalkina, N. S.; Kashapova, L. K.
2009SPD....40.1920K    Altcode:
  We investigate accelerated electron energy spectra for different sources
  in a large flare using simultaneous observations obtained with two
  instruments, the Nobeyama Radio Heliograph (NoRH) at 17 and 34 GHz,
  and the Reuven Ramaty High Energy Solar Spectroscopic Imager (RHESSI)
  at hard X-rays. This flare is one of the few in which emission up to
  energies exceeding 200 keV can be imaged in hard X-rays. Furthermore,
  we can investigate the spectra of individual sources up to this
  energy. We discuss and compare the HXR and microwave spectra and
  morphology. Although the event overall appears to correspond to the
  standard scenario with magnetic reconnection under an eruptive filament,
  several of its features do not seem to be consistent with popular flare
  models. In particular we find that (1) microwave emissions might be
  optically thick at high frequencies despite a low peak frequency in
  the total flux radio spectrum, presumably due to the inhomogeneity
  of the emitting source; (2) magnetic fields in high-frequency radio
  sources might be stronger than sometimes assumed; (3) sources spread
  over a very large volume can show matching evolution in their hard
  X-ray spectra that may provide a challenge to acceleration models. Our
  results emphasize the importance of studies of sunspot-associated flares
  and total flux measurements of radio bursts in the millimeter range.

---------------------------------------------------------
Title: Forecasting the velocity of quasi-stationary solar wind and
    the intensity of geomagnetic disturbances produced by it
Authors: Eselevich, V. G.; Fainshtein, V. G.; Rudenko, G. V.;
   Eselevich, M. V.; Kashapova, L. K.
2009CosRe..47...95E    Altcode:
  A brief review is given of contemporary approaches to solving the
  problem of medium-term forecast of the velocity of quasi-stationary
  solar wind (SW) and of the intensity of geomagnetic disturbances caused
  by it. At the present time, two promising models of calculating
  the velocity of quasi-stationary SW at the Earth’s orbit are
  realized. One model is the semi-empirical model of Wang-Sheeley-Arge
  (WSA) which allows one to calculate the dependence V( t) of SW velocity
  at the Earth’s orbit using measured values of the photospheric
  magnetic field. This model is based on calculation of the local
  divergence f <SUB>S</SUB> of magnetic field lines. The second model
  is semi-empirical model by Eselevich-Fainshtein-Rudenko (EFR). It
  is based on calculation in a potential approximation of the area
  of foot points on the solar surface of open magnetic tubes (sources
  of fast quasistationary SW). The new Bd-technology is used in these
  calculations, allowing one to calculate instantaneous distributions of
  the magnetic field above the entire visible surface of the Sun. Using
  predicted V( t) profiles, one can in EFR model calculate also the
  intensity of geomagnetic disturbances caused by quasi-stationary
  SW. This intensity is expressed through the K <SUB> p </SUB> index. In
  this paper the EFR model is discussed in detail. Some examples of
  epignosis and real forecast of V( t) and K <SUB> p </SUB>( t) are
  discussed. A comparison of the results of applying these two models
  for the SW velocity forecasting is presented.

---------------------------------------------------------
Title: Microwave observations with the RATAN-600 radio telescope:
    detection of the thermal emission sources
Authors: Grigoryeva, Irina Yu.; Kashapova, Larisa K.; Livshits,
   Moisey A.; Borovik, Valery N.
2009IAUS..257..177G    Altcode:
  We report on two off-limb radio sources of microwave emission
  which were detected in one-dimensional RATAN-600 solar scans of the
  post-eruptive loops: on December 2, 2003 (off west limb) and January
  25, 2007 (east limb). The microwave spectra showed that the thermal
  emission was predominant at the early stage of the arcade formation
  with a small contribution of non-thermal emission. There were no
  high-energy particles in these events. The microwave spectra of the
  radio sources associated with the tops of postflare loops show the
  predominant thermal emission during one hour after the eruption. In case
  of a small contribution from accelerated particles to the microwave
  emission, there is a large amount of hot plasma in the region of the
  loop tops after the eruption.

---------------------------------------------------------
Title: A Possible Scenario of Energy Transport in the 17<SUP>th</SUP>
    May 2002 Flare
Authors: Kotrč, P.; Kashapova, L. K.; Frolova, A. S.; Kuprjakov,
   Yu. A.
2009CEAB...33..207K    Altcode:
  We deduce the energy transport scenario from simultaneous observations
  in a wide range of the electromagnetic spectrum. High-temporal
  resolution optical and radio spectra from the Ondřejov observatory,
  and data obtained by RHESSI, Nobeyama Radio Observatory, Radio Solar
  Telescope Network (RSTN) and by SOHO (MDI and EIT) were analysed to
  get a complex view on the event. As follows from the microwave data the
  maximum of emission at 17 GHz evolved from the eastern part of the flare
  to the western one. Chromospheric emission of the flare originated from
  two eruptive centres -- eastern and western ones. While the eastern
  centre consisted of a single Hα kernel, the western one was rather
  a complex structure. These centres were associated with different
  HXR sources. The western centre was connected with a more mighty HXR
  source of 25-100 keV. We studied a correlation of the hard X-rays,
  radio emission and the Balmer series lines for the western centre
  in detail. Probable agents and scenarios of the energy transport
  are discussed.

---------------------------------------------------------
Title: Eruptive processes at the beginning of development of powerful
    flare-active regions on the sun
Authors: Kashapova, L. K.; Livshits, M. A.
2008ARep...52.1015K    Altcode: 2008AZh....85.1129K
  The evolution of large solar activity centers is studied, and
  the conditions resulting in powerful nonstationary processes are
  clarified. In addition to the factors that are usually considered
  (changes in sunspot area, the structure of magnetic fields, the
  character of motions), we examine to what extent observations of
  nonstationary processes (flares and associated coronal mass ejections)
  can be used to predict the development of such processes in the
  subsequent evolution of the activity center. We considered the example
  of a powerful group in October 2003, which could be observed before
  its appearance at the eastern limb using a spacecraft in near-Mars
  orbit. We plotted for events occurring in 2003 images of flares in
  various spectral ranges and analyzed high-energy processes in group
  486, which was isolated at the beginning of its development, and then
  in the interrelated groups 486 and 484. The analysis of the peculiar
  early development of group 486 suggested that an intensification of the
  activity could be expected due to the emergence of new magnetic flux
  (and satellite groups), as well as the interaction and synchronization
  of two and then three large groups of the end of October 2003. In
  other words, in this case, extremely powerful nonstationary processes
  are associated with a relatively higher contribution of large-scale
  magnetic fields. We compare our results to analyses of motions and
  magnetic fields in this activity center throughout its transit across
  the disk from October 23 to November 5, 2003.

---------------------------------------------------------
Title: Non-thermal particle effects on the Hα and Hβ line profiles
    in the 18 August 2002 solar flare
Authors: Kashapova, L. K.; Kotrč, P.; Kupryakov, Yu. A.
2008AnGeo..26.2975K    Altcode:
  We present results of the 18 August 2002 flare analysis as an example
  for developing a diagnostic tool for thermal and non-thermal processes
  in chromospheric lines. Taking into account the hard X-ray (HXR)
  emission, we attempted to derive the Hα and Hβ line properties which
  were caused by the non-thermal electron contribution and could be useful
  for diagnostic purposes. The flare itself was a sequence of harder and
  softer bursts in HXR and we investigated three flare kernels associated
  with them. Two of the kernels appeared simultaneously. This phase of
  the flare could be observed in a broad band of wavelengths (HXR, UV,
  optical and microwaves). Kernel 1 did not clearly coincide with any
  HXR source but its intensity increased with the HXR flux rise. The
  flare kernel~3 did not show any significant response in microwaves,
  however, the related HXR flux was comparable with the flux of the
  previous kernels. We carried out an analysis of the difference between
  the Hα/Hβ profile rate in the line center at the distance of 0.5 Å
  from the line center. Only kernel 2 showed parameter fluctuations that
  were related to HXR flux evolution. The supposition of the non-thermal
  electron effect on the Hα/Hβ profile ratio was confirmed only at
  the kernel connected with the 25 50 keV HXR source. We found further
  confirmation that the Hα/Hβ line intensity ratio could be used as
  a diagnostic tool for non-thermal electron presence.

---------------------------------------------------------
Title: An Extreme Solar Event of 20 January 2005: Properties of the
    Flare and the Origin of Energetic Particles
Authors: Grechnev, V. V.; Kurt, V. G.; Chertok, I. M.; Uralov,
   A. M.; Nakajima, H.; Altyntsev, A. T.; Belov, A. V.; Yushkov, B. Yu.;
   Kuznetsov, S. N.; Kashapova, L. K.; Meshalkina, N. S.; Prestage, N. P.
2008SoPh..252..149G    Altcode: 2008arXiv0806.4424G; 2008SoPh..tmp..145G
  The famous extreme solar and particle event of 20 January 2005 is
  analyzed from two perspectives. Firstly, using multi-spectral data,
  we study temporal, spectral, and spatial features of the main phase
  of the flare, when the strongest emissions from microwaves up to 200
  MeV gamma-rays were observed. Secondly, we relate our results to a
  long-standing controversy on the origin of solar energetic particles
  (SEP) arriving at Earth, i.e., acceleration in flares, or shocks
  ahead of coronal mass ejections (CMEs). Our analysis shows that
  all electromagnetic emissions from microwaves up to 2.22 MeV line
  gamma-rays during the main flare phase originated within a compact
  structure located just above sunspot umbrae. In particular, a huge
  (≈ 10<SUP>5</SUP> sfu) radio burst with a high frequency maximum
  at 30 GHz was observed, indicating the presence of a large number of
  energetic electrons in very strong magnetic fields. Thus, protons and
  electrons responsible for various flare emissions during its main phase
  were accelerated within the magnetic field of the active region. The
  leading, impulsive parts of the ground-level enhancement (GLE),
  and highest-energy gamma-rays identified with π<SUP>0</SUP>-decay
  emission, are similar and closely correspond in time. The origin of
  the π<SUP>0</SUP>-decay gamma-rays is argued to be the same as that
  of lower-energy emissions, although this is not proven. On the other
  hand, we estimate the sky-plane speed of the CME to be 2 000 - 2 600
  km s<SUP>−1</SUP>, i.e., high, but of the same order as preceding
  non-GLE-related CMEs from the same active region. Hence, the flare
  itself rather than the CME appears to determine the extreme nature of
  this event. We therefore conclude that the acceleration, at least, to
  sub-relativistic energies, of electrons and protons, responsible for
  both the major flare emissions and the leading spike of SEP/GLE by 07
  UT, are likely to have occurred nearly simultaneously within the flare
  region. However, our analysis does not rule out a probable contribution
  from particles accelerated in the CME-driven shock for the leading
  GLE spike, which seemed to dominate at later stages of the SEP event.

---------------------------------------------------------
Title: On Fast Chromospheric Responses to Microwave Subsecond Bursts
Authors: Kashapova, L. K.; Kotrc, P.; Meshalkina, N. S.
2008ESPM...12.2.47K    Altcode:
  We present a multi-wavelength analysis of chromosphere responses
  produced during the subsecond bursts detected by Siberian Solar Radio
  Telescope (SSRT, 5.7 GHz) on April 26, 2003 at 08:05:30 UT. The data
  obtained by Nobeyama Radioheliograph (NoRH, 17 and 34 GHz), Ondrejov
  observatory and RHESSI were also used. A correlation of multi-wavelength
  observations (microwave emission, hard X-rays and the video-cadence
  chromospheric line spectra from the Ondrejov observatory obtained with
  0.04 second resolution) was performed to study fluxes on various levels
  of solar atmosphere before, during and after the event. The temporal
  resolution was high enough to resolve responses to subsecond pulses in
  the individual correlated fluxes and their possible interrelations. The
  results and possible scenario are briefly discussed from point of view
  of the energy transport mechanisms.

---------------------------------------------------------
Title: On Dynamics of H-alpha/H-beta Line Ratio and Non-thermal
    Particle Effects in Solar Flares
Authors: Kotrc, P.; Kashapova, L. K.; Kuprjakov, Yu. A.
2008ESPM...12.2.61K    Altcode:
  The ratio of the H-alpha?/H-beta line profiles was analyzed as
  a diagnostic indicator of non-thermal particle effects in solar
  flares. Differences between the H-alpha/H-beta profile ratio in the line
  center and at the distance of 0.5 Angstroms from the line center were
  studied in various phases of flares as concerns presence of responses
  to non-thermal effects. Variations of this parameter were compared
  with the HXR flux evolution for the 26 June 1999 and the 18 August
  2002 solar flares. The sign of the parameter changed from negative
  to positive value only for these flare kernels where coincidence with
  the HXR sources indicated presence of accelerated particles. However,
  no such a change was found for the other kernels. <P />The revealed
  effect was compared with information obtained from correlation between
  the temporal fluctuations of the H? and H? line and the HXR flux. <P
  />The obtained results are discussed from point of view of their
  possible diagnostical applications.

---------------------------------------------------------
Title: On the Total Emissivity in Chromospheric Lines in the 17th
    May 2002 Flare
Authors: Prosecky, T.; Kotrc, P.; Kashapova, L. K.
2008ESPM...12.2.63P    Altcode:
  Energy balance in the 17th May 2002 flare was studied. Chromospheric
  lines observed by the Ondrejov spectrograph were analysed taking into
  account the HXR data from RHESSI. Positions of the HXR sources were
  identified at the H-alpha slit-jaw images and the corresponding flare
  spectra were processed. Total emissivity in H-alpha and H-beta lines was
  derived and the net energy emitted in these lines during various phases
  of the flare was estimated. The results were compared with evolution
  of HXR flux and plasma parameters obtained from the HXR spectra.

---------------------------------------------------------
Title: On Energy Transport Scenarios in the 17th May 2002 Near-limb
    Flare
Authors: Kotrc, P.; Kashapova, L. K.; Frolova, A. S.; Kuprjakov, A. Yu.
2008ESPM...12.2.62K    Altcode:
  We present a reconstruction of the energy transport scenario based
  on the simultaneous observations in a wide range of electromagnetic
  spectrum. Particularly, the high-temporal resolution optical and radio
  spectra from the Ondrejov observatory, data obtained by RHESSI, Nobeyama
  Radio Observatory, Radio Solar Telescope Network (RSTN), Siberian
  Solar Radio Telescope (SSRT) and SOHO (MDI and EIT) were analysed to
  obtain a complex view on the event. Especial attention was payed to
  the role of accelerated particles in the energy transport and to the
  excitation mechanisms in different kernels of the flare. As follows from
  the microwave data the maximum of emission at 17 GHz evolved from the
  eastern part of the flare to the western one. On chromospheric level
  the flare consisted of two eruptive centers - eastern and western
  ones. While the eastern center consisted from a single H? kernel,
  the western one was rather a complex structure. These centers were
  associated with different HXR sources. It is worth to note that the
  western center was connected with a more mighty HXR source of 25-100
  keV. <P />We studied a correlation of the hard X-rays, radio emission
  and the Balmer series lines for the western center. Probable agents
  and scenarios of the energy transport as well as possible diagnostic
  aspects of the results are briefly discussed.

---------------------------------------------------------
Title: Multi-wavelength investigation of energy release and transport
    in the 16 August 2004 flare
Authors: Kashapova, L. K.; Zharkova, V. V.; Grechnev, V. V.; Ipson,
   S. S.
2008IAUS..247..222K    Altcode: 2007IAUS..247..222K
  The current contribution investigates the solar flare of 16th August
  2004 with the multi-wavelength observations with high temporal
  resolution from RHESSI, Large Solar Vacuum Telescope (LSVT), Hiraiso
  Solar observatory, Nobeyama Radioheliograph (NoRH, 17 and 34 GHz) and
  Siberian Solar Radio Telescope (SSRT, 5.7 GHz), TRACE. The main flare
  was preceded by a pre-flare event with a very short energy release
  time. The observations of the main flare reveal a close temporal
  correlation between the Hα intensity observed with LSVT and those in
  hard and soft X-ray emissions observed with RHESSI, and in microwave
  fluxes observed with NoRH and SSRT. This close temporal correlation can
  be only associated with high-energy particles. The role of energetic
  particles in energy transport and non-thermal excitation and ionisation
  on Hα emission during the pre-flare and pre-flare event is investigated
  with full non-LTE approach and possible agents and scenarios of energy
  transport are discussed.

---------------------------------------------------------
Title: Balmer-Line Diagnostics of Accelerated Particles
Authors: Kashapova, L. K.; Kotrč, P.; Kupryakov, Yu. A.
2007ASPC..368..431K    Altcode:
  Preliminary results of empirical study of a non-thermal electron effect
  on Hα/Hβ line intensity ratio in solar flares are presented. Analysis
  of spectral observations of the 26 June 1999 flare revealed some
  peculiarities of the Hα/Hβ line intensity ratio (the “sidelobes”)
  in the emission kernels associated with radio bursts and HXR emission
  that could be considered as an indirect evidence of accelerated
  non-thermal particle beams. According to our conclusions they appeared
  due to non-thermal electron beam effects. Consequently, the obtained
  results confirmed the theoretical predictions and bore a first witness
  for a detection of the spatial and temporal presence or absence of
  the non-thermal electron beams in optical spectra. However, as a more
  statistically probative evidence was needed, we extended our analysis
  on two flares where presence of non-thermal mechanisms of excitation
  was verified by HXR data. The obtained results are quite promising as
  concerns of diagnostics of the energy release and transfer mechanisms
  during the flare.

---------------------------------------------------------
Title: Signatures of High-Energy Particles in Hα Emission Before
    the Solar Flare of August 16, 2004
Authors: Kashapova, L. K.; Zharkova, V. V.; Grechnev, V. V.
2007ASPC..368..437K    Altcode:
  We study multi-spectral chromospheric and coronal emissions that
  appeared during the impulsive event occurring before the flare on
  16 August 2004 observed by RHESSI, Large Solar Vacuum Telescope
  (Irkutsk), and Nobeyama Radioheliograph (NoRH, 17 and 34 GHz). There
  are three separate sources detected: 1 in hard X-rays (RHESSI), two
  in microwaves (NoRH) (1 of which coincides with HXR) and one in Hα
  emission (3). The emission in all sources reveals a close (within 1 s)
  temporal correlation that can be only associated with precipitation
  of high-energy particles. Possible scenarios of particle precipitation
  and its effect on the observed signatures are discussed.

---------------------------------------------------------
Title: The multi-wavelength study of the effect of energetic particle
    beams on the chromospheric emission in the 25th July 2004 solar flare
Authors: Zharkova, V. V.; Kashapova, L. K.; Chornogor, S. N.;
   Andriyenko, O. V.
2007AdSpR..39.1483Z    Altcode:
  We present the multi-wavelength study of short-term variations of
  Hα line emission located in multiple kernels on the both sides from
  magnetic neutral line in the 25th July 2004 solar flare observed by VTT
  (Tenerife). The HXR and Hα emission in the kernels 1 and 3 is close
  spatially and temporally while in kernels 4 and 7 there is only delayed
  Hα emission observed tens seconds after HXR in the kernels 1 and 3. The
  locations of Hα kernels 1, 3, 4 and 7 are on the opposite sides from
  the magnetic neutral line. The temporal variations of Hα emission in
  kernels 1 and 3 coincide within 5 s with the HXR photon emission. The
  latter is found to have double power law photon spectra, which were
  corrected to a single power law with the turning point technique
  accounting for Ohmic losses and collisions. The Hα emission is fit by
  full non-LTE simulations in an atmosphere heated by an electron beam
  with the parameters derived from the HXR emission. The combination
  of radiative, thermal and non-thermal mechanisms of excitation and
  ionization of hydrogen atoms is considered. The temporal evolution of
  simulated Hα emission in the kernel 3 fits rather well the two observed
  intensity increases: the first at the flare onset (13:38:39-13:39:30 UT)
  caused by pure non-thermal excitation by beam electrons and the second
  one appearing after 13:40:00 UT because of a hydrodynamic heating. The
  observed close temporal correlation or delay of Hα emission with HXR
  emission points out to the precipitation either of electron (kernels
  1 and 3) or protons (4 and 7).

---------------------------------------------------------
Title: On the thermal and non-thermal excitation effects as studied in
    the H[alpha], H[beta] and Ca II 8542 Å line profiles in a solar flare
Authors: Kotrč, P.; Kashapova, L. K.
2007msfa.conf..277K    Altcode:
  Spectral observations of the 26 June 1999 flare (Kotrč et al. 2004)
  presented a unique opportunity to compare effects of thermal and
  non-thermal mechanisms of excitation on profiles of Balmer series and Ca
  II 8542 A lines. The radio spectra and HXR flux demonstrated indirect
  evidence of the non-thermal beam effect on the chromosphere during
  the flare (Kashapova et al. 2005). We compared the line profiles in
  the flare kernel associated with the influence of non-thermal electron
  beams with the "only thermal" kernels. Results are discussed both from
  their observational and theoretical aspects.

---------------------------------------------------------
Title: Signatures of High Energy Particle Beams in the Chromospheric
    Events Before the 25 July 2004 Flare Onset
Authors: Kashapova, L. K.; Zharkova, V. V.; Chornogo, S. N.; Kotrc, P.
2006IAUJD...1E..47K    Altcode:
  A role of particle beams is studied in the origin and evolution
  of small-scale chromospheric events appeared before the main phase
  onset at 13:37 UT of the July 25, 2004 flare. The main goal of our
  investigation was to detect possible locations of energy release and to
  trace the processes of energy transport by high-energy particles to the
  chromosphere. Based on the plasma and beam parameters deduced from hard
  X-ray flux and UV data, 1D hydrodynamic responses of the atmosphere
  is calculated and used for a full non-LTE simulation of hydrogen
  H-alpha line emission taking into account thermal and non-thermal
  processes. Theoretical line profiles are compared with the observed
  dynamics of H-alpha intensity. A comparison is carried out of the
  high energy particle parameters deduced from chromospheric emission,
  hard X-ray flux and UV data that allows us to find a possible scenario
  of the event evolution.

---------------------------------------------------------
Title: On Possible Manifestation of Non-Thermal Electrons in the
    Hα/Hβ Line Profile Ratio in the June 26, 1999 Flare
Authors: Kotrc, P.; Kashapova, L. K.
2006IAUJD...1E..46K    Altcode:
  We analyzed the solar flare on 26 June 1999 which consisted of three
  subsequent phases. All of them were followed by events of quite
  different types (Kotrc et al., IAU Symp 223, 2004). Just the second
  phase of the flare was accompanied by radio bursts and HXR emission
  that could be considered as an indirect evidence of accelerated
  non-thermal particle beams. Theoretical calculations of thermal
  mechanisms coupled with accelerated electron beams in flares showed
  that the ratio of the Hα/Hβ line profiles could be a possible
  indicator whether a mechanism of non-thermal radiation excitation
  was present or absent (Kasparova &amp; Heinzel, A&amp;A, 2002). This
  effect should follow the occurrence of the particle beams in time
  and then decay. In the flare kernel associated thus possibly with
  the influence of non-thermal electron beams we found that the ratio
  of the Hα/Hβ line profiles demonstrated a very specific form which
  substantially differs from those ones obtained in "thermal" kernels
  (occurring in the first and in the another flare phases). This effect
  can be characterized by presence of specific "sidelobes" occurring in
  the ratio of the line profiles. The effect was observed in the region
  nearby the HXR sourcelocation where it appeared just after the end of
  the radio-spectrum spike and therefore it corresponds most probably to
  the occurrence of non-thermal processes in the flare. The associated
  HXR effect was rather short lasting, i.e. the effect of "sidelobes"
  disappeared earlier then the emission. We try to trace the evolution and
  the possible decay of this effect. On one hand the obtained results will
  be an additional evidence of the theoretical predictions, on the other
  hand they could be useful for development of technique for detecting
  the presence or absence of the non-thermal electron beams. Conclusions
  are discussed both from their observational and theoretical aspects.

---------------------------------------------------------
Title: The evolution of Hα and CaII K emission before and during
    the solar M-class flare on 25th July 2004
Authors: Chornogor, S. N.; Kashapova, L. K.; Andriyenko, O. V.
2006IAUS..233..122C    Altcode:
  The last decade observations revealed the essential variations of energy
  balance take place in the pre-flare active regions at all atmospheric
  levels and they are caused by both evolution of AR and processes
  associated with flare activity. We present the multi-wavelength study
  of the solar flare jointly with the preceding event. The combined
  investigation is perspective for the mechanism understanding of the
  energy storage, trigger and release during the solar flares. A special
  attention was given to signatures of energetic particle beam effect on
  chromosphere according to Hα and CaII K intensity changes. Combination
  of data from ground based instruments and space observatories (TRACE,
  MDI, RHESSI) will allow us to track processes taking place in a wide
  range of solar atmosphere layers - from the temperature minimum region
  to the corona. The obtained results are discussed.

---------------------------------------------------------
Title: Investigation of pre-flare role of Ellerman bombs in solar
    active regions
Authors: Papernaya, Yu. V.; Kashapova, L. K.
2006IAUS..233..181P    Altcode:
  Ellerman bombs or moustache are known as short-living fine
  emission structures associated with a local energy release in solar
  atmosphere. The relation between the moustaches and flare has been
  discussed since the moment of the moustaches discovery. The resent
  results of the Flare Genesis Experiment demonstrated that this problem
  is still actual and attractive. We took into account the possibility
  of different mechanisms of their origin (thermal and non-thermal) by
  using spectro polarimetric data obtained in summer 1999 and carried
  out analysis of Ellerman bomb's role in flare activity of the Sun by
  the example of the several active regions.

---------------------------------------------------------
Title: The multi-wavelength study of the effect of energetic particle
    beams on the chromospheric emission in the 20th and 25th July 2004
    solar flares
Authors: Zharkova, V. V.; Andriyenko, O. V.; Chornogor, S. N.;
   Kashapova, L. K.; Sych, R. A.
2006cosp...36.2256Z    Altcode: 2006cosp.meet.2256Z
  We present the results of a multi-wavelength study of short-term
  variations of H-alpha and CaII K line emission in the 20th and 25th July
  2004 solar flares In both flares the fast changes of H-alpha and CaII
  K intensity observed from VTT correlated very closely seconds with the
  HXR emission observed by RHESSI that is considered as the signatures
  of energetic particle beams in the chromosphere For interpretation
  of the observed emission the full non-LTE radiative simulations were
  carried out for a combination of radiative thermal and non-thermal
  mechanisms of excitation and ionization of the hydrogen and Ca emission
  in flaring atmospheres Various theoretical models are compared with the
  observational results in order to define the best fits and to clarify
  the processes of energy transport within a short timescale of seconds
  from upper to lower atmospheric levels in the solar flares

---------------------------------------------------------
Title: On AN Effect of Particle Beams on Correlation Between Balmer
    Series Lines
Authors: Kashapova, L. K.; Kotrč, P.; Kupryakov, Yu. A.; Kašparová,
   J.
2005ESASP.600E.126K    Altcode: 2005dysu.confE.126K; 2005ESPM...11..126K
  No abstract at ADS

---------------------------------------------------------
Title: Preflare HXR and Chromospheric Line Emission in NOAA 0652 ON
    25TH July 2004
Authors: Chornogor, S. N.; Kashapova, L. K.; Sych, R. A.; Andriyenko,
   O. V.
2005ESASP.600E.115C    Altcode: 2005dysu.confE.115C; 2005ESPM...11..115C
  No abstract at ADS

---------------------------------------------------------
Title: The viewing angle effect on Hα-line impact polarisation in
    impulsive solar events
Authors: Zharkova, V. V.; Kashapova, L. K.
2005A&A...431.1075Z    Altcode:
  The effect of a viewing angle on the hydroden Hα-line impact
  polarisation is investigated in a plane vertical atmosphere arbitrary
  located on the solar disk. The impact polarisation is assumed
  to be caused by precipitating beam electrons with pitch-angular
  anisotropy steadily injected into the flaring atmosphere from its
  top. The polarisation is calculated for a 3 level plus continuum
  hydrogen atom affected by Zeeman splitting in a moderate magnetic
  field taking into account depolarising effects of diffusive radiation
  and collisions with thermal electrons. The Hα polarisation profiles
  are affected by electron beams only in the line cores whereas the
  wings are fully depolarized by the collisions with thermal electrons
  despite the extended wing emission, or “moustaches”, caused by
  beam electrons. The full (integrated in wavelength) Hα-line linear
  polarisation, caused by moderate electron beams, is shown to be 2{-}20%
  and either negative or positive depending on the position of a flaring
  loop on the solar disk and the direction of an emitted photon from
  the local magnetic field. The polarisation plane is projected onto
  a viewing angle psi, being a superposition of the flare location
  on a solar disk and the magnetic field deviation from vertical on
  the solar surface. For viewing angles less then 50^circ the Hα-line
  impact polarisation is negative increasing up to -10% towards smaller
  angles, meaning that the polarisation is mostly perpendicular to the
  plane {B}× {K} where B is the magnetic field induction and K is the
  photon momentum vector. For viewing angles greater than 60^circ the
  measured impact polarisation becomes positive, sharply increasing up
  to 20% towards the limb. In the range of 50{-}60^circ the observed
  impact polarisation goes through a zero point despite the actual
  presence of beam electrons in the flaring atmosphere. The theoretical
  predictions of the dependence of polarisation degree on viewing angle
  fit remarkably well the observations of Hα-line linear polarisation
  in small-scale flaring events such as moustaches or Ellerman bombs,
  located in different positions on a solar disk.

---------------------------------------------------------
Title: Transfer of energy within coronal bright points according to
    the observation in optical spectra and microwave
Authors: Prosovetsky, D. V.; Kashapova, L. K.
2004IAUS..223..479P    Altcode: 2005IAUS..223..479P
  The paper is devoted to the coronal bright points. We carried out
  the analysis of the simultaneous observations in IR He λ10830 Å and
  microwaves at 5.2 and 1.76 cm. It was obtained that microwave sources
  correspond to the dark points in IR He λ10830 Å with line-of-sight
  velocities directed from a observer. The possible mechanism of the
  energy transport within the bright points are suggested.

---------------------------------------------------------
Title: On the presence of linear polarization in the flare on 26
    June, 1999
Authors: Kotrc, P.; Kashapova, L. K.; Kupryakov, J. A.
2004IAUS..223..463K    Altcode: 2005IAUS..223..463K
  Solar flare on 26 June 1999 was accompanied by radio bursts giving
  an indirect evidence of accelerated superthermal particle beams. It
  is generally believed that this effect can stimulate an impact linear
  polarization in Balmer series spectral lines. The flare was observed
  simultaneously by the Ondrejov Multichannel Flare Spectrograph (MFS)
  and by the Large Solar Vacuum Telescope (LSVT) using the polarization
  optics in the Halpha line. Spectropolarimetric data obtained by the two
  instruments are analyzed, however no substantial linear polarization
  was detected. Both spectral and auxiliary data, including radio and
  X-ray observations are analyzed to discuss possible reasons of the
  lack of linear polarization.

---------------------------------------------------------
Title: Polarization of Ellerman bombs and the arch structure of
active region: some results of investigation
Authors: Kashapova, L. K.
2004IAUS..223..459K    Altcode: 2005IAUS..223..459K
  The comparison of the polarization presence in Ellerman bombs or
  moustaches and the active region arch structure was carried out. In the
  most cases of the polarization, interpreted as impact polarization, were
  detected in that regions where the bright small loops were observed. On
  the contrary, when a significant polarization wasn't detected the
  scanning during observation was carried out nearby the large loops.

---------------------------------------------------------
Title: Spectropolarimetric Investigation of Hα Line Profiles in
    Moustaches
Authors: Kashapova, L. K.
2003ASPC..307..474K    Altcode:
  No abstract at ADS

---------------------------------------------------------
Title: Some results of the spectropolarimetric investigation of
    Ellerman bombs
Authors: Kashapova, L. K.
2002ESASP.506..661K    Altcode: 2002svco.conf..661K; 2002ESPM...10..661K
  Ellerman bombs (EB) or moustaches are enigmatic phenomena of solar
  atmosphere and mechanisms of their excitation are still unclear. There
  are two main models of their explanation. Thermal model implies the
  compression and heating of small regions of solar atmosphere. According
  to the non-thermal model the beams of energetic particles are considered
  as the source of EB origin. If the EB have thermal origin, then there
  is a large possibility that they will show a prominent center-to limb
  variation of the Hα line profiles. The Hα line polarization would
  be about 2-3% both in the line core and in the wings. The moustaches
  arisen as the result of bombardment by energetic particle beams will
  show a polarization observed in the Hα line core only. The form of
  these Hα line profiles would correlate with their life time. The
  contribution presents an investigation of the Hα line profiles in
  EB which showed the polarization of different types. We also make
  an attempt to analyse correlation between the life time and the form
  of the Hα line profiles obtained for three long-living moustaches,
  which showed significant linear polarization in the line core.

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Title: Measurement and processing of linear polarization in solar
    flares - a comparison of two methods
Authors: Kotrč, P.; Firstova, N. M.; Kashapova, L. K.; Kupryakov,
   Yu. A.
2002ESASP.506..947K    Altcode: 2002svco.conf..947K; 2002ESPM...10..947K
  Linear polarization measurement in solar flares is discussed from the
  point of view of the processing technique. Usually, spectropolarimetric
  investigation of the linear polarization in solar flares is carried
  out for the line profiles. The results obtained by two methods
  (either processing of individual profiles or the whole spectral
  strips) are compared and applied to the observations obtained at the
  Large Solar Vacuum Telescope (the Baikal Astrophysial obseratory)
  and at the Ondřejov Multichannel Flare Spectrograph. The results
  obtained by the second method are comparable by accuracy with the
  results obtained by the first one. Moreover, it allows to check the
  instrumental polarization and the polarization behaviour in the nearby
  objects. However, the profile operating method allows to investigate
  the polarization effects along the dispersion more carefully.

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Title: On the possible manifestation of the solar G-mode in the
    Earth atmosphere
Authors: Klochek, N. V.; Nikonova, M. V.; Kashapova, L. K.; Sotnikova,
   R. T.
2002ESASP.506..153K    Altcode: 2002ESPM...10..153K; 2002svco.conf..153K
  The Sun influences the processes occurred in the Earth's atmosphere
  and interplanetary space by means of not only electromagnetic but
  presumably gravitational forces. As it was reported by a group of
  researches (Thomson, D. et al.) charged particles in the interplanetary
  medium reveal variations with periods approaching theoretically expected
  periods of solar g-modes. It is believed that the detected periodicities
  are an indirect manifestation of these modes. Special attention was paid
  to the quasi-two-day periodicity of 2.2 days. To investigate its origin
  these authors carried out an analysis of atmospheric pressure variations
  which reveals the 2.2 day periodicity. We are justified in anticipating
  a manifestation of characteristic properties of this periodicity in
  space and in time. The wave process in the Earth's atmosphere with a
  typical quasi-two-day period reveals the quadrupole structure which
  seems to be the response to the effect of the low-frequency g-mode of
  the Sun.

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Title: A Spectropolarimetric Study of Ellerman Bombs
Authors: Kashapova, L. K.
2002ARep...46..918K    Altcode:
  We have studied four 10 to 40 minute sets of Hα spectropolarimetric
  observations of five Ellerman bombs (a total of 241 spectropolarimetric
  recordings) selected from data for more than 200 Ellerman bombs obtained
  with the Large Solar Vacuum Telescope at the Ba kal Astrophysical
  Observatory. The degree of polarization P and azimuth of the plane
  of polarization were derived from quasi-simultaneous observations of
  the Stokes parameters Q/I and U/I. We interpret the observed linear
  polarization as impact polarization. A method for comparing the
  polarization parameters of Ellerman bombs observed at different times
  and distances from the center of the solar disk is suggested, which can
  be used to relate variations of the polarimetric parameters with the
  lifetimes of Ellerman bombs. A comparison between the observations and
  theoretical calculations indicates that the observed Ellerman bombs
  were due to electron beams with energies of several hundred keV.

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Title: Observation of the linear polarization in the flare with a
    powerful surge
Authors: Firstova, N. M.; Kashapova, L. K.
2002A&A...388L..17F    Altcode:
  An investigation of the linear polarization in the flare with a
  powerful surge revealed an unusual behavior of the Stokes parameter
  profiles along the dispersion. We discuss the probability that photons
  propagating from the flare and passing through the surge generate a
  linearly polarized radiation of the surge.

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Title: The results of spectropolarimetric observations of solar
    flares followed by surge
Authors: Firstova, N. M.; Kashapova, L. K.
2002ESASP.477..103F    Altcode: 2002scsw.conf..103F
  An investigation of the linear polarization in the June 29, 1999 flare
  with a powerful surge (the maximum velocity was about 160 km/sec)
  revealed an unusual behavior of the Stokes parameter profiles along the
  dispersion. We discuss the probability that photons propagating from
  the flare and passing through the surge generate a linearly polarized
  radiation of the surge.

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Title: Investigation of He I 10 830 Å `Dark Points' at the Sayan
    Solar Observatory and the Baikal Astrophysical Observatory
Authors: Skomorovsky, V. I.; Firstova, N. M.; Kashapova, L. K.;
   Kushtal, G. I.; Boulatov, A. V.
2001SoPh..199...37S    Altcode:
  A new two-bandpass birefringent filter has been produced at
  ISTP, Irkutsk for the investigation of the fine structure of the
  chromosphere. One filter passband is centered on the He i 10 830 Å
  line, the second one is centered on Hα. The FWHM of the He i 10 830 Å
  passband is 0.46 Å and of the Hα passband is 0.3 Å. A large number of
  filtergrams were obtained with the filter at the Sayan observatory. At
  the same time, spectral observations with high spatial and spectral
  resolution were carried out by the large solar vacuum telescope at the
  Baikal Observatory. We selected 29 `dark point' spectra with sizes from
  2” to 13”, as well as `dark points' on the filtergrams. Comparison of
  spectrograms and filtergrams has shown a good agreement of their size
  and intensity in relation with the surrounding chromosphere as well
  as the absence of primary line-of-sight velocities in both observation
  types. From spectral observations, the depth of 10 830 Å is over 30%
  for some `dark points', and the FWHM is more than 1 Å. He i 10 830 Å
  line profiles in `dark points' are more deep and wide than in quiet
  regions. The optical depth of the chromosphere in `dark points' is
  estimated. Comparison with the unperturbed chromosphere showed that
  `dark points' in He i 10 830 Å are more optically thin than the
  nearby chromosphere.

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Title: The Today's Investigations on Large Solar Vacuum Telescope
Authors: Skomorovsky, V. I.; Firstova, N. M.; Kashapova, L. K.;
   Firstova, A. V.; Kushtal, G. I.
2001AGM....18.P221S    Altcode:
  The contribution presents the prospective observations obtained with
  the Large Solar Vacuum Telescope (Baikal astrophysical observatory,
  Irkutsk) from 1997 after its re-equipment by CCD-camera. During the
  latest years we carried out basically the spectropolarimetric Hα
  observations of the emission objects of different sizes from the solar
  flares to the Ellerman bombs. The flares followed by a surges have
  aroused a special interest. The observations and preliminary results are
  shown. The Ellerman bombs or moustaches were devoted much attention. We
  obtained the extensive observational data( more than 200 objects) and
  the various mechanisms of their arising have been analyzed. Besides
  the investigation of the linear polarization in Hα line the spectral
  observations in IR region (HeI 10830 Å line) were carried out. Also
  we obtain the observation of the pores in the several Fe lines for the
  latest two years. This work was supported by Russian Foundation for
  Basic Research grants 00-02-16068-a and 01-02-06203. Thanks are also
  due the State Support of Leading Scientific Schools of the Russian
  Federation grant 00-15-96659 and the State Scientific and Technical
  Program “Astronomy” for their support.

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Title: Program for the 1999 August 11 eclipse
Authors: Grigoriev, V. M.; Eselevich, V. G.; Kashapova, L. K.;
   Salakhutdinov, R. T.; Skomorovsky, V. I.
1999CoSka..28..256G    Altcode:
  A study of the solar coronal fine structure up to 5--6 solar radii
  as an indicator of the global and local processes on the Sun. The
  experimental detection of fast changes in coronal structures. An
  investigation of the minimal and maximal coronal structure (streamer
  form) as a result of the plasma layer projection on the picture plane
  along the neutral line. Obtaining 8--10 images of the white-light corona
  with the radial neutral filter. The special telescope was developed
  and manufactured. The telescope tube is directed to (or from) the
  polar star. The Sun's tracking is carried out by the whole telescope
  tube with the heliostat mirror around the polar axis. The lens of the
  telescope is a two-component Petzval type, the diameter is 120 mm,
  and the focal length is 1200 mm. The assumed angular resolution at the
  region +/-2.5 degree is near 5 arcsec. Data will be recorded either
  via an automatic 8-cm aerial camera or using a CCD-detector.

---------------------------------------------------------
Title: The linear polarization in moustaches
Authors: Firstova, N. M.; Boulatov, A. V.; Kashapova, L. K.
1999ASSL..243..451F    Altcode: 1999sopo.conf..451F
  No abstract at ADS

---------------------------------------------------------
Title: A spectropolarimetric study of the Hα radiation from
    Ellerman bombs.
Authors: Kazantsev, S. A.; Firstova, N. M.; Kashapova, L. K.; Bulatov,
   A. V.; Petrashen', A. G.
1998RuPhJ..41.1258K    Altcode:
  Polarization data are given for three whiskers recorded with the
  large solar vacuum telescope at Baikal Observatory, Institute of
  Solar-Terrestrial Physics, Russian Academy of Sciences. The observed
  degree of polarization varies from 2 to 13%. The direction of the
  polarization plane for the medium intensity whisker was tangential,
  while that for the weakest one was radial. The brightest whisker had
  a polarization plane direction close to radial at the center of the
  line but tangential at the flanks. It is assumed that the polarization
  is due to impact excitation of a hydrogen-atom ensemble in the solar
  chromosphere by an electron beam, and estimates are made of the
  beam energy.

---------------------------------------------------------
Title: Spectropolarimetric studies of H<SUB> alpha </SUB> emission
in "solar moustaches": Observations and calculation of the Stokes
    parameters
Authors: Kazantsev, S. A.; Firstova, N. M.; Kashapova, L. K.; Bulatov,
   A. V.; Petrashen', A. G.; Henoux, J. -C.
1998ARep...42..702K    Altcode:
  The results of spectropolarimetric observations of three solar
  `moustaches' carried out on the Large Vacuum Solar Telescope of
  Baikal Observatory of the Institute of Solar-Terrestrial Physics are
  presented. The observed degree of polarization varies from 2-13%. The
  direction of the plane of polarization for a moustache with moderate
  intensity is tangential, and is radial for the weakest moustache. In
  the brightest moustache, the plane of polarization is close to radial
  at the line center, and is tangential in the wings.

---------------------------------------------------------
Title: A program of Observations for the August 11, 1999 Total
    Solar Eclipse
Authors: Grigoriev, V. M.; Eselevich, V. G.; Kashapova, L. K.;
   Salakhutdinov, R. T.; Skomorovsky, V. I.
1998jena.conf...12G    Altcode:
  A study of the solar coronal fine structure up to 5--6 solar radii
  as an indicator of the global and local processes on the Sun. The
  experimental detection of fast changes in coronal structures. An
  investigation of the minimal and maximal coronal structure (streamer
  form) as a result of the plasma layer projection on the picture plane
  along the neutral line. Obtaining 8--10 images of the white-light corona
  with the radial neutral filter. The special telescope was developed
  and manufactured. The telescope tube is directed to (or from) the
  polar star. The Sun's tracking is carried out by the whole telescope
  tube with the heliostat mirror around the polar axis. The lens of the
  telescope is a two-component Petzval type, the diameter is 120 mm,
  and the focal length is 1200 mm. The assumed angular resolution at the
  region ±2.5 degree is near 5 arcsec. Data will be recorded either
  via an automatic 8-cm aerial camera or using a CCD-detector.

---------------------------------------------------------
Title: Image Processing of Digitized Spectral Data
Authors: Boulatov, A. V.; Kashapova, L. K.
1998ASPC..145...63B    Altcode: 1998adass...7...63B
  Every observatory has a library of old pictures taken by photographic
  cameras. These measurements are not as such high quality as those
  from modern CCD systems, but could contain important data about
  rare phenomena or source data for long-period investigations (e.g.,
  concerning the solar cycle). This paper presents methods for converting
  photographic images, collected at the Large Solar Vacuum Telescope
  (Baikal Astrophysical Observatory) to digital images, similar to CCD
  pictures. Special algorithms were used for this task and have been
  implemented in the IDL environment. The results of processing real
  spectral data and a comparison of processed photographic images and
  images taken with a TEK CCD are presented.