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Author name code: antalova
ADS astronomy entries on 2022-09-14
author:"Antalova, Anna" 

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Title: Hysteresis between solar flare index and cosmic rays during
    the past three solar cycles, 20, 21, and 22
Authors: Ozguc, A.; Antalova, A.; Atac, T.
2002cosp...34E.513O    Altcode: 2002cosp.meetE.513O
  We study the hysteresis effect between the solar flare index and cosmic
  ray intensity for the last three solar cycles. We show that smoothed
  time series of flare index and cosmic ray intensity exhibit significant
  solar cycle dependent differences in their relative variations during
  the studied period. The shapes of these differences vary from cycle to
  cycle. So we investigate the momentary time lag between the two time
  series for the odd and even cycles. As a prediction of the behavior of
  the hysteresis for the current cycle, the values of the flare index
  and the cosmic ray intensities of the ascending branch of cycle 23
  were added to the plots.

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Title: Time Evolution of low-Frequency Periodicities in Cosmic
    ray Intensity
Authors: Kudela, K.; Rybák, J.; Antalová, A.; Storini, M.
2002SoPh..205..165K    Altcode:
  The long-time series of daily means of cosmic-ray intensity observed by
  four neutron monitors at different cutoff rigidities (Calgary, Climax,
  Lomnický Štít and Huancayo/Haleakala) were analyzed by means of
  the wavelet transform method in the period range ∼ 60 to ∼ 1000
  days. The contributions of the time evolution of three quasi-periodic
  cosmic-ray signals (∼ 150 d, ∼ 1.3 yr and ∼ 1.7 yr) to the
  global one are obtained. While the ∼ 1.7-yr quasi-periodicity, the
  most remarkable one in the studied interval, strongly contributes to
  the cosmic ray intensity profile of solar cycle 21 (particularly in
  1982), the ∼ 1.3-yr one, which is better correlated with the same
  periodicity of the interplanetary magnetic field strength, is present
  as a characteristic feature for the decreasing phases of the cycles
  20 and 22. Transitions between these quasi-periodicities are seen in
  the wavelet power spectra plots. Obtained results support the claimed
  difference in the solar activity evolution during odd and even solar
  activity cycles.

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Title: Comparing wavelet and traditional studies in the Gnevyshev
    Gap context
Authors: Storini, M.; Laurenza, M.; Rybak, J.; Antalova, A.; Kudela, K.
2002cosp...34E2174S    Altcode: 2002cosp.meetE2174S
  As it is now well established the Gnevyshev Gap is a significant
  phenomenon of the solar activity maxima (e.g. [1-3]) and Wavelet
  Transform Method allows to investigate non-stationary processes
  containing multi-scale features. Results from such kind of method
  applied to several parameters of the Solar-Terrestrial System are
  used together with the ones from traditional investigation methods to
  better understand controversial findings obtained during the maximum
  phase of the last four solar activity cycles. [1] F. Feminella and
  M. Storini (1997), Astron. Astrophys. 322, 311. [2] G.A. Bazilevskaya
  et al. (2000), Solar Phys. 197, 157. [3] M. Storini et al. (2002),
  Adv. Space Res., in press.

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Title: On the quasi-biennial modulation of galactic cosmic rays
Authors: Storini, M.; Rybak, J.; Antalova, A.; Kudela, K.
2001ICRC....9.3768S    Altcode: 2001ICRC...27.3768S
  Results from the wavelet power spectrum (WPS) analysis of the cosmic
  ray intensity, registered by the Calgary neutron monitor from 1969 to
  1998 years, are used to discuss the characteristic behaviour of the
  quasi-biennial modulation of galactic cosmic rays during solar activity
  cycles n. 21 and n. 22. Results from the temporarily averaged global
  power spectra (GPS) are also shown.

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Title: On the wavelet approach to cosmic ray variability
Authors: Kudela, K.; Storini, M.; Antalova, A.; Rybák, J.
2001ICRC....9.3773K    Altcode: 2001ICRC...27.3773K
  A wavelet transform (time scale ~60 to ~1000 days) is applied on the
  long-term time series of daily means of cosmic ray intensity observed
  by neutron monitors at different cutoff rigidities. No persistent
  periodicities with the same amplitude are found for the whole period
  analyzed. The temporal evolution of quasiperiodic variations at
  ~150 days, ~1.3 years and ~1.7 years is examined. While the ~1.7-y
  quasiperiodicity (the most remarkable one in the studied interval) is
  strongly contributing to the cosmic ray intensity profile of solar cycle
  21 (particularly in 1982), the ~1.3-y one (which is better correlated
  with the same periodicity of the interplanetary magnetic field strength)
  is a characteristic feature for the decreasing phases of the cycles 20
  and 22. Transitions between them are seen from the wavelet power spectra
  plots. Obtained results give a support to the claimed difference in
  the solar activity evolution during odd and even solar activity cycles.

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Title: The Solar and Cosmic-Ray Synodic Periodicity (1969 1998)
Authors: Antalová, A.; Kudela, K.; Rybák, J.
2001SSRv...97..355A    Altcode:
  The synodic recurrence of the Mt. Wilson plage index (MPSI) and the
  Calgary cosmic ray (CR) intensity is investigated, using the wavelet
  power spectra in the range of 18 38 days, during the last three solar
  cycles. The unique temporal coincidence between the quasi synodic MPSI
  and the CR periods is detected in 1978 1982 (the 21st solar cycle). In
  the 22nd cycle there is a very strong MPSI synodic recurrence, from
  1989.5 to 1990.5, but it is absent in the CR data. In 1992.5 1993.5
  the MPSI and CR recurrence phenomenon is in good accordance with the
  solar wind speed and cosmic ray modulation as measured during the
  first Ulysses passage around the Sun. The Gnevyshev gap is present in
  the 27-day recurrence of CR, in agreement with Kudela et al. (1999).

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Title: The Wavelet Analysis of the Solar and Cosmic-Ray Data
Authors: Rybák, J.; Antalová, A.; Storini, M.
2001SSRv...97..359R    Altcode:
  Results of the wavelet power spectrum (WPS) analysis(which covers
  the 1969 1998 years) obtained using the daily data of the following
  parameters: (i) the Mt. Wilson Magnetic Plage Strength index (MPSI),
  (ii) the solar LDE-type flare index (LDE-FI) and (iii) the Calgary
  cosmic-ray (CR) intensity, are reported for periods ranging between
  64 and 1024 days. The temporal distribution of the WPS during the
  last three solar activity cycles is extremely discontinuous. A clear
  resemblance between the CR and LDE-FI WPS is obtained only for the
  22nd solar activity cycle. Nevertheless, the CR multiperiod peak,
  observed in 1982, can well be identified with the WPS peaks obtained
  in both solar parameters under consideration. In the 21st cycle, we
  found significant the MPSI periods around 850 880 days (2.3 2.4 yr),
  while such periods are present in the LDE-FI data of the 22nd cycle. In
  the CR data we discerned a net periodicity around 650 days (1.7 yr).

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Title: Daily soft X-ray flare indices (1985 and 1986)
Authors: Antalova, A.
2001CoSkS..31...51A    Altcode:
  The heliographic longitudinal distribution of the daily soft X-ray flare
  index values (FI) is given for 1985 and 1986 years (Table 1). The FI
  was determined from the daily continuous SMS-GOES profile of solar
  soft X-ray flux (0.1-0.8 nm), as published in Solar Geophysical
  Data. The left (right) columns of Table 1 comprise the 1985 (1986)
  daily data. The Eastern (-E), Central (-C) and Western (-W) LDE-type
  FIs, as well as, a daily flare index computed from the impulsive-type
  (I) flares were so far published for the decreasing part of the 20-th
  solar cycle, as well as for the 21-st solar cycle.

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Title: Cosmic ray/Soft X-ray background relationship from July 1968
    to June 1987
Authors: Jakimiec, M.; Antalova, A.; Storini, M.
2000CoSka..30...75J    Altcode:
  The cross-correlation technique has been applied to obtain quantitative
  information on the short-term relation between the intensity of the
  nucleonic component of galactic cosmic rays (CR), as recorded by the
  Calgary neutron monitor, and the solar soft X-ray background (XBG),
  measured by satellites. The data consisted of uninterrupted daily
  sequences from July 1968 to June 1987. Using the 12-month basic (b_i),
  detrended (d_i), the running mean (m_i(n)) and the residual sequences
  (r_i(n)), where n = 3, 7, 15, 27 days and i = 1,..., 19, the consecutive
  CR/XBG cross-correlation functions (ccf-s) were computed with a time lag
  ranging from -2 to +60 days. In 13 cases out of the 19 d_i sequences,
  a statistically significant anticorrelation was found in the first
  minimum (for a lag shorter than or equal to 10 days). The m_i and
  the r_i sequences helped to identify fluctuations on different time
  scales. In Jakimiec, Antalova and Storini (1999) results for the period
  July 1968-June 1980 were used to underline differences and analogies
  between the descending phase of solar activity cycle n. 20 and the
  ascending phase of solar activity cycle n. 21, i.e., one complete
  heliomagnetic semicycle. Here we mainly compared the relationship
  between both parameters during two consecutive descending phases of
  cycle n. 20 with the one of cycle n. 21.

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Title: Daily soft X-ray flare indices (1983 and 1984).
Authors: Antalová, A.
2000CoSka..30...43A    Altcode:
  The heliographic longitudinal distribution of the daily soft X-ray
  flare indices is given for 1983 and 1984. The soft X-ray flare index
  was determined from the daily continuous SMS-GOES profile of solar
  soft X-ray flux, as published in Solar Geophysical Data.

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Title: Daily soft X-ray flare indices (1983 and 1984)
Authors: Antalova, A.
2000CoSkS..30...43A    Altcode:
  The heliographic longitudinal distribution (-E, -C and -W) of the daily
  soft X-ray flare indices is given for 1983 (the left E--T columns)
  and 1984 years (the right E-T columns of Table 1). The soft X-ray flare
  index was determined from the daily continuous SMS-GOES profile of solar
  soft X-ray flux (0.1-0.8 nm), as published in Solar Geophysical Data.

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Title: Effects of Hysteresis of Some Solar Indices during the Past
    Three Solar Cycles 20, 21 and 22
Authors: Özgüç, A.; Atac, T.; Antalova, A.
2000ESASP.463..403O    Altcode: 2000sctc.proc..403O
  No abstract at ADS

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Title: Variability of the CR/XBG-L Relationship during the Solar
    Cycle Evolution
Authors: Jakimiec, M.; Antalova, Anna; Storini, Marisa
2000ESASP.463..337J    Altcode: 2000sctc.proc..337J
  No abstract at ADS

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Title: The Variations of the Solar Activity and the Low Rigidity
    Cosmic Rays (1969-1998)
Authors: Antalová, A.; Kudela, Karel; Rybak, Jan
2000ESASP.463..281A    Altcode: 2000sctc.proc..281A
  No abstract at ADS

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Title: The Intermittency of the Solar Intermediate-Term Periodicity
    (1969-1998)
Authors: Rybák, J.; Antalova, Anna; Storini, Marisa
2000ESASP.463..419R    Altcode: 2000sctc.proc..419R
  No abstract at ADS

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Title: Synodic Recurrency of Cosmic Rays
Authors: Antalová, A.; Kudela, K.; Langer, R.
1999ESASP.448.1125A    Altcode: 1999ESPM....9.1125A; 1999mfsp.conf.1125A
  No abstract at ADS

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Title: Fourier Analysis of the LDE-type Flare Occurrence (1969 - 1997)
Authors: Antalová, A.
1999ESASP.448..743A    Altcode: 1999ESPM....9..743A; 1999mfsp.conf..743A
  No abstract at ADS

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Title: Cosmic-ray intensity versus solar soft X-ray background in
    cross-correlation analysis
Authors: Jakimiec, Maria; Antalová, Anna; Storini, Marisa
1999SoPh..189..373J    Altcode:
  The relationship between the galactic cosmic ray modulation (CR)
  and the non-flare coronal level, as given by the solar soft X-ray
  background (XBG), is investigated from 1 July 1968 to 30 June 1980 on
  a daily basis. The stationarity problem of a multivariate time series,
  as well as the role of the short- and medium-term corona variability
  are faced. From them it is found that the CR/XBG relation is variable
  during the considered heliomagnetic semicycle, while CR and XBG are
  highly anticorrelated on a long-time scale (12-month averages). The
  CR/XBG relationship during the declining phase of solar activity shows
  a moderately strong anticorrelation, on short- and medium-term time
  scales (coefficient up to −0.77 for 27-day running averages), went
  towards insignificant values in the minimum phase and is only partially
  reconstructed during the rise of the following solar cycle. During
  the solar activity maximum of cycle 20 the cosmic-ray modulation is
  only related to the short-term coronal fluctuations (no other time
  scales are significant, supporting the reliability of the so-called
  `Gnevyshev gap' in solar parameters).

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Title: Soft X-ray flare indices in 1981 and 1982 years
Authors: Antalova, A.
1999CoSkS..29..163A    Altcode:
  The heliographic longitudinal distribution of the daily soft X-ray
  flare index (FI) values is given for 1981 and 1982 years (Table 1). The
  days, when FI exceeds the value 500 (300) are indicators of extremely
  large LDE activity and they are as follows: 1979 - 3 (6) days; 1980 -
  3 (12); 1981 - 6 (16) and maximum in 1982 - 8 (16) days. The FI was
  determined from the daily continuous SMS-GOES profile of the solar
  soft X-ray flux (0.1-0.8 nm), as published in SGD. The left (right)
  columns of Table 1 comprise the 1981 (1982) daily data. The Eastern
  (E), Central (C) and Western (W) distribution of the LDE--type FIs,
  as well as a daily FI computed from the impulsive (I)-type flares,
  were so far published from 1969 to 1982.

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Title: Daily soft X-ray flare indices (1979 and 1980)
Authors: Antalova, A.
1999CoSkS..29...59A    Altcode:
  The heliographic longitudinal distribution of the daily soft X-ray
  flare index values is given for 1979 and 1980 years (Table 1). The soft
  X-ray flare index was determined from the daily continuous SMS-GOES
  profile of solar soft X-ray flux (0.1-0.8 nm), as published in Solar
  Geophysical Data. The left (right) columns of Table 1 comprise the
  1979 (1980) daily data. The Eastern (E), Central (C) and Western (W)
  LDE-type flare indices, as well as a daily flare index computed from
  the impulsive-type (I) flares were so far published for the decreasing
  part of the 20-th solar cycle, as well as for the onset part of the
  21-st solar cycle (from January 1, 1969 to December 31, 1980).

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Title: Daily soft X-ray flare indices (1979 and 1980).
Authors: Antalová, A.
1999CoSka..29...59A    Altcode:
  The heliographic longitudinal distribution of the daily soft X-ray flare
  index values is given for 1979 and 1980 years. The soft X-ray flare
  index was determined from the daily continuous SMS-GOES profile of solar
  soft X-ray flux (0.1 - 0.8 nm), as published in Solar Geophysical Data.

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Title: On the double-peaked cycle of solar activity: a connection
    with the heliomagnetic field.
Authors: Storini, M.; Feminella, F.; Antalová, A.; Massetti, S.
1999joso.proc..153S    Altcode:
  After a careful study of several solar activity parameters, Feminella
  and Storini (1997) showed the reliability of the double-peak structure
  for the 11-year solar activity cycle (Gnevyshev, 1977 and references
  therein), when intense and/or long-lasting activity events are
  considered. In particular, an evident link between the occurrence of
  major solar events and the strength of the heliomagnetic field energy
  was found for cycle n. 21. Magnetic field data from the solar telescope
  of the Stanford University (Web pages) and from the Huairou Station
  (Bao and Zhang, 1998) are used to reinforce the previous interpretation.

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Title: Lomnický Štít and Calgary cosmic ray measurments during
    the 22-nd solar cycle.
Authors: Antalová, A.; Kudela, K.; Langer, R.
1999joso.proc..201A    Altcode:
  The authors report on the solar cycle trend obtained from the CA/LS
  correlation functions of the galactic cosmic ray intensity daily data.

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Title: LDE-type events in solar soft X-rays (1986 year).
Authors: Antalová, A.
1999joso.proc..199A    Altcode:
  A small number of the Long Duration coronal Events (LDE) favored 1986
  year for the detailed study of connection of solar SXR activity to
  short-term Cosmic Ray (CR) modulation. The best 1986 cross-correlation
  functions were found in CR versus XBG data. The solar XBG (X-BackGround)
  reflects the longitudinal distribution of the large-scale magnetic
  fields (MF) in the solar corona and further this Sun's MF distribution
  induces the magnetic morphology of the inner heliosphere.

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Title: Coronal mass ejections, flares, and geomagnetic storms
Authors: Landi, R.; Moreno, G.; Storini, M.; Antalová, A.
1998JGR...10320553L    Altcode:
  We investigate the role of the coronal mass ejections (CMEs) (by using
  soft X ray solar emission as proxy data) in producing the nonrecurrent
  geomagnetic storms in the period 1969-1974. The linkage between these
  phenomena is confirmed: however, it turns out that CMEs associated
  with chromospheric flares, accompanied by type 4 radio emission,
  are the most effective in perturbing the geomagnetic field.

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Title: 1977 and 1978 daily soft X-ray flare indices
Authors: Antalova, A.
1998CoSkS..28...63A    Altcode:
  The heliographic longitudinal distribution of the daily soft X-ray
  flare index values is given for 1977-1978 years (Table 1). The soft
  X-ray flare index was determined from the daily continuous SMS-GOES
  profile of solar soft X-ray flux (0.1-0.8 nm), as published in Solar
  Geophysical Data. The left (right) columns of Table 1 comprise the
  1977 (1978) daily data. The Eastern (E), Central (C) and Western (W)
  LDE-type flare indices, as well as a daily flare index of the impulsive
  (I) flares were published for the decreasing part of the 20-th solar
  cycle, as well as for the onset part of the 21-st solar cycle (from
  January 1, 1969 to December 31, 1978).

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Title: 1977 and 1978 daily soft X-ray flare indices.
Authors: Antalová, A.
1998CoSka..28...63A    Altcode:
  The heliographic longitudinal distribution of the daily soft X-ray
  flare index values is given for 1977 - 1978. The soft X-ray flare
  index was determined from the daily continuous SMS-GOES profile of
  solar soft X-ray flux, as published in Solar Geophysical Data.

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Title: The LDE flares (1969-1990)
Authors: Antalová, A.; Viktorínová, B.
1998PAICz..88...75A    Altcode:
  No abstract at ADS

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Title: June 26, 1983, 14:07 UT 300 keV, 3B/M7 east-limb solar flare
Authors: Antalová, A.; Ogir, M. B.
1998PAICz..88...71A    Altcode:
  No abstract at ADS

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Title: Spatial and temporal distribution of the LDE-type flares.
Authors: Antalová, A.
1998joso.proc..162A    Altcode:
  The spatial and temporal distributions of the Strongest LDE-type
  Flaring Centers (SFCs) are investigated between 1969 and 1995 using
  synoptic maps of coronal magnetic fields at the source surface,
  prepared at Wilcox Solar Observatory. An SFC is, by definition, any
  flaring center whose LDE-type flare index exceeds value 1000. There
  were the 14 flare-richest active regions of the ascending phase of the
  21-st cycle (from 1977 to 1980) and from them 10 SFCs are related to
  the reversed magnetic sectors and 4 SFCs to their boundaries. Out of
  15 outstanding LDE-type flaring centers of the 22-nd cycles 10 SFCs are
  located along the source surface neutral line, 5 SFCs were found inside
  the reversed magnetic polarity sectors and none in old polarity sectors.

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Title: On Time Lags Between Soft X-ray Flares and Galactic CR
    Modulation (1969-1976)
Authors: Antalová, A.; Jakimiec, M.; Storini, M.
1998asct.conf..475A    Altcode:
  No abstract at ADS

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Title: 22nd Cycle's Sectorial Distribution of LDE-type Flaring Centers
Authors: Antalová, A.
1998asct.conf..117A    Altcode:
  No abstract at ADS

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Title: Solar soft X-ray parameters: 1969-1976 autocorrelation
    functions
Authors: Jakimiec, M.; Storini, M.; Antalova, A.
1997CoSka..27..104J    Altcode:
  The autocorrelation analysis of solar soft X-ray parameters was
  performed with a time lag ranging from 1 to 32 days (acf_j, with j=1,
  ..., 32) for the 1969-76 period. Consecutive sequences containing
  daily data for a 2-year interval were considered. From the comparison
  of the autocorrelation functions for both flare (TOT) and nonflare
  (XBG) soft X-ray variables we selected the different recurrent
  tendency over the years. During the maximum (1969-71) and minimum
  (1975-76) phases of the 20th solar cycle the recurrency of all
  the SXR parameters is included between 18 and 23 days, but during
  the decreasing activity phase (1972-74) recurrencies approach the
  expected 27-day synodic rate of rotation. The nonflare X-ray corona
  has a particularly stable 27-day recurrency (from 1971-72 to 1974-75),
  but the flare TOT variable displays the 27-day recurrency only in the
  1972-73 sequence (Figure 5). The most stable 25-day TOT recurrency was
  observed in 1973-75. Our results of the atypical "solar periodicity"
  of TOT values (i.e., acf_lm < 27 days) are in agreement with past
  findings based on other solar activity indices and cycles. However,
  we have also noted, on a short time scale (1 day), that there exists
  a strong coherence (acf_1 ~ 0.8) of the XBG variables for all the
  investigated intervals. While this coherence is high (acf_1 ~ 0.7)
  in the TOT variable only for 1973-75, when long-lived coronal holes
  covered a large fraction of the solar surface, in the other periods
  the parameter acf_1(TOT) =< 0.55. The above findings were never
  explicitly emphasized in solar soft X-ray studies.

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Title: The 20-th solar cycle minimum and its daily soft X-ray flare
    index (1975-1976)
Authors: Antalova, A.
1997CoSkS..27..129A    Altcode:
  The longitudinal distribution of the daily soft X-ray flare index is
  given for 1975-1976 years. The soft X-ray flare index was determined
  from the daily continuous GOES profile of solar soft X-ray flux
  (0.1--0.8 nm), as published in Solar Geophysical Data. The Eastern
  (E), Central (C) and Western (W) LDE-type flare indices, as well as
  a daily flare index of the impulsive (I) flares at present cover the
  decreasing part of the 20--th solar cycle (from January 1, 1969 to
  December 31, 1976).

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Title: The 20th solar cycle minimum and its daily soft X-ray flare
    index (1975 - 1976).
Authors: Antalová, A.
1997CoSka..27..129A    Altcode:
  The longitudinal distribution of the daily soft X-ray flare index is
  given for 1975 - 1976. The soft X-ray flare index was determined from
  the daily continuous GOES profile of solar soft X-ray flux (0.1 -
  0.8 nm), as published in Solar Geophysical Data.

---------------------------------------------------------
Title: The continuation of the daily soft X-ray flare index
    (1973-1974)
Authors: Antalova, A.
1997CoSka..27...31A    Altcode:
  The daily soft X-ray flare index was determined from the daily
  continuous profile of solar soft X-ray flux, as published in Solar
  Geophysical Data. In order to determine the heliographic coordinates
  of Long Duration Events (LDEs) we exploited the fact that the
  soft X-ray flare emission is uniquely tied with the occurrence of
  H-alpha flares. The daily flare index is given in Table 1. The left
  (right) columns of Table 1 comprise the 1973 (1974) year data. Table
  1 contains the Eastern (E), Central (C) and Western (W) indices of
  an LDE as well as a daily flare index of the impulsive (I) flares,
  observed from January 1, 1973 to December 31, 1974.

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Title: Multivariate daily sequence analyses of GCR/solar X-ray
    parameters
Authors: Jakimiec, M.; Storini, M.; Antalová, A.
1997AdSpR..20..111J    Altcode:
  Cross-correlation analyses between Calgary neutron monitor data and
  soft (1-8 A˚ X-ray parameters (derived from SOLRAD measurements)
  were performed on daily basis for the maximum phase of solar cycle
  20. Clues for a strong relationship between X-ray solar flares and
  cosmic ray modulation in time were not found.

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Title: To Forecast Huge Forbush Decreases During Solar Activity Cycles
Authors: Storini, M.; Massetti, S.; Antalova, A.
1997ICRC....1..409S    Altcode: 1997ICRC...25a.409S
  No abstract at ADS

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Title: Daily soft X-ray flare index (1969-1972)
Authors: Antalova, A.
1996CoSka..26...98A    Altcode:
  The daily soft X-ray flare index was determined from the daily
  continuous profile of solar soft X-ray flux. In order to determine the
  heliographic coordinates of Long Duration Events (LDEs) we exploited
  the fact that the soft X-ray flare emission is uniquely tied with
  the occurrence of H-alpha flares. The daily flare index is given in
  Tables 1 and 2. They contain the Eastern (E), Central (C) and Western
  (W) indices of an LDE as well as a daily flare index of the impulsive
  (I) flares, observed from January 1969 to December 1972.

---------------------------------------------------------
Title: The magnetic reversal of the 21st solar cycle and LDE-type
    flares
Authors: Antalová, A.
1996AdSpR..17d.213A    Altcode: 1996AdSpR..17..213A
  The spatial and temporal distributions of LDE-type flaring regions
  are investigated for 42 solar rotations between the years 1977 and
  1980 using synoptic maps of the coronal magnetic field at the source
  surface, prepared at Wilcox Solar Observatory. 14 outstanding LDE-type
  flaring centers are found to be distributed not at random but mostly
  inside the large-scale solar sectors of reversed magnetic polarity
  (10 centers), as well as at their boundaries (4 centers).

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Title: Long Duration Soft X-ray Events and Galactic Cosmic Ray
    Modulation
Authors: Antalova, A.; Rybak, J.; Kudela, K.; Venkatesan, D.
1996ASPC...95..119A    Altcode: 1996sdit.conf..119A
  No abstract at ADS

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Title: Magnetic Reversal in the 22nd Solar Cycle and Spatial
    Distribution of LDE-type Flares
Authors: Antalova, A.; Jakimiec, M.
1996ASPC...95...82A    Altcode: 1996sdit.conf...82A
  No abstract at ADS

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Title: Catalogue of LDE-type flares (1994 - 1995).
Authors: Antalová, A.
1996CoSka..26...65A    Altcode:
  The Catalogue of LDE-type flares covers 27 years of LDE-type flare data
  (1969 - 1995). The continuation of the list of long-lasting SXR flares
  (LDE-type) is given.

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Title: Galactic Cosmic Ray Modulatton and Solar X-ray Parameters
    During the Maximum Phases of Sunspot Cycles 20 and 22
Authors: Antalova, A.; Storini, M.; Jakimiec, M.
1996ASPC...95..437A    Altcode: 1996sdit.conf..437A
  No abstract at ADS

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Title: LDE-type flares and heliosphere (1969 - 1995).
Authors: Antalová, A.
1996joso.proc..106A    Altcode:
  The aim of this paper is to evaluate a possible connection between the
  Galactic cosmic ray modulation in the heliosphere and solar outward
  directed phenomena by extending previous intercorrelation analysis on
  a daily basis.

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Title: Solar neutron measurements on the Solar Probe
Authors: Kudela, K.; Kuznetsov, S. N.; Antalová, A.
1996AdSpR..17c..49K    Altcode: 1996AdSpR..17Q..49K
  We outline briefly possibilities for measurement of solar neutrons on
  the Solar Probe and their relevance for understanding acceleration
  processes at the solar surface, based on the current status of the
  solar neutron investigation and some of the devices used until now.

---------------------------------------------------------
Title: Catalogue of LDE-type flares (1994-1995)
Authors: Antalova, A.
1996CoSkS..26...65A    Altcode:
  The Catalogue of LDE-type flares covers 27 years of LDE-type flare data
  (1969 - 1995). The continuation of the list of long-lasting SXR flares
  (LDE-type) is given in Table 1. The latter contains the list of LDE
  flares observed from July 1994 to June 1995, and ties in timewise with
  the previous papers; it is only available in a "computer-file" form.

---------------------------------------------------------
Title: On the correlation between daily GCR intensity values and
    LDE-type flare index (1987, 1988, 1990 and 1992)
Authors: Antalova, A.; Kudela, K.; Venkatesan, D.; Rybak, J.
1995AdSpR..16i.233A    Altcode: 1995AdSpR..16..233A
  The correlation analysis between daily values of Calgary Galactic
  Cosmic Ray intensity (CNI) and LDE-type flare index (FI) reveals
  the following results: in all years under consideration, the CNI-FI
  anticorrelation is small, but statistically significant. The yearly
  CNI-FI trend depends on yearly heliospherical conditions and on their
  22-year cyclical changes. At the onset of the 22-nd cycle (in 1987) the
  CNI-FI relation had broad minimum, similar to the result for non-flare
  SXR background corona in 1987. In 1988 and 1992 the typical short-term
  CNI-FI lag (from - 1 to - 3 days) was found, indicating the presence
  of local heliospherical CNI modulation sources. In 1990, the CNI-FI
  correlation has two comparable, large minima at - 22 as well as -
  9 day CNI lags. Such double peak form of the 1990's CNI-FI minimum
  is consistent with the existence of two, amplitudinally balanced CNI
  modulation sources in the 1990's heliosphere. The first source seems
  to be a substantial Global Merged Interaction Region (GMIR) located
  in the outer heliosphere (producing the - 22 day CNI lag). The second
  source was a typical local heliospherical structure, indicated by
  short-term CNI lags.

---------------------------------------------------------
Title: Daily values of the solar SXR background and modulation of GCRs
    (1987, 1988, 1990 and 1992)
Authors: Antalova, A.; Kudela, K.; Venkatesan, D.; Rybak, J.
1995AdSpR..16i.237A    Altcode: 1995AdSpR..16..237A
  We present here the results of the intercorrelation analysis between
  the daily Calgary Galactic Cosmic Ray intensity values (CNI) and daily
  solar SXR background (XBG - unresolved full-sun SXR GOES flux). The
  anticorrelation between CNI and XBG is statistically significant
  for 1987, 1988 and 1992 sequences. In 1990, no anticorrelation
  between CNI and XBG was found. The latter fact gives evidence for
  the Global Merged Interaction Region (GMIR) being the most dominant
  GCR modulation structure of the 1990's outer heliospherical system,
  while local heliospherical structures seemed to play the secondary role.

---------------------------------------------------------
Title: Daily Values of the Solar SXR Background and Galactic Cosmic
    Ray Modulation (1968-1972)
Authors: Antalová, A.; Rybák, J.; Kudela, K.; Venkatesan, D.
1995ICRC....4..534A    Altcode: 1995ICRC...24d.534A
  No abstract at ADS

---------------------------------------------------------
Title: Sectorial Distribution of LDE-Type Flares
Authors: Antalová, A.; Jakimiec, M.
1995ICRC....4...70A    Altcode: 1995ICRC...24d..70A
  No abstract at ADS

---------------------------------------------------------
Title: Catalogue of LDE-type flares (1993 - 1994).
Authors: Antalová, A.
1995CoSka..25..121A    Altcode:
  The Catalogue of LDE-type flares covers 25 years of LDE-type flare data
  (1969 - 1994). This paper lists LDE flares observed from July 1993 to
  June 1994.

---------------------------------------------------------
Title: Solar magnetic sectors and spatial distribution of LDE-type
    flares
Authors: Antalova, A.; Jakimiec, M.
1995CoSka..25...19A    Altcode:
  We present a number of statistical tests that speak in favour of
  an increased (both LDE-type and impulsive) flare activity in active
  regions (ARs) which are located inside or along the boundaries of the
  solar sectors with `reversed' magnetic polarity. Altogether 338 daily
  values of 32 BEARALERT regions have been analysed in terms of eight
  variables during the ascending phase of the 22nd solar cycle. The
  flare occurrence is found smallest inside the `old' sectors and peaks
  inside the `reversed' sectors and at the sectors' boundaries. Separate
  analyses of the data showing a lack of strong flare activity for a
  given day (the data subset dn, comprising 155 daily vectors), and
  the data pertinent to strong flare activity in a given day (the data
  subset df, representing 183 daily vectors) lead to the same results
  concerning the sectorial distribution of active regions.

---------------------------------------------------------
Title: Catalogue of LDE-type flares (19931994)
Authors: Antalova, A.
1995CoSkS..25..121A    Altcode:
  The Catalogue of LDE-type flares covers 25 years of LDE-type flare data
  (1969-1994). The continuation of the list of long-lasting SXR flares
  (LDE-type) is given in Table 1. The latter contains the list of LDE
  flares observed from July 1993 to June 1994, and ties in timewise
  with the previous paper (Antalova 1990); it is only available in
  a computer-file form. One considers temporal variations of the
  occurrence of the LDE flares, with SXR duration exceeding 2 hours,
  throughout the 22-nd cycle. Current studies of the heliosphere regard
  Coronal Mass Ejections (CMEs) as a principal phenomenon modifying
  its properties. CMEs are usually accompanied by dynamic activity
  phenomena (LDE-type flares, DBs and eruptive prominences). That is
  the reason why CMEs are implicitly incorporated in LDE-type flare
  list. Analysis of the LDE-type flare occurrence in solar cycles 20,
  21 and 22 is published in the following papers: -- Periodicities
  of the LDE-type flare occurrence (1969-1992) in Antalova (1994). --
  Cosmic-ray modulation and long-duration solar flare events, in Kudela
  et al. (1994). -- On the correlation between daily GCR intensity values
  and LDE-type flare index (1987, 1988, 1990 and 1992) in Antalova et
  al. (1995). The temporal changes found in a daily CNI-FI anticorrelation
  profile reflect the cyclic magnetic reversal of the Sun as well as the
  corresponding heliospherical topology. -- E-W distribution of Solar
  LDE-type Flares and Galactic Cosmic ray modulation (1969-1972) in
  Antalova et al. (1994) and Jakimiec et al. (1995). -- Role of LDE-type
  flares in the GCR Modulation (1969-1972) in Antalova et al. (1995) --
  The magnetic reversal in the 21st solar cycle and LDE-type flares in
  Antalova (1996).

---------------------------------------------------------
Title: Contributions of the Astronomical Observatory Skalnate Pleso,
    Volume 25
Authors: Zverko, Juraj; Antalova, Anna; Svoren, Jan; Chochol, Drahomir;
   Kucera, Ales; Porubcan, Vladimir
1995STIN...9624442Z    Altcode:
  Topics addressed include astrometry of minor planets, solar magnetic
  sectors and spatial distribution of LDE-type flares, radar observations
  of the Perseid meteor shower, periodic variations in the light
  curves of symbiotic stars, photometry of symbiotic stars, even-odd
  solar-cycle differences of corona brightness, solar eclipses, and index
  of cosmic ray fluctuations at neutron monitor energies. Also addressed
  is stratification of chromium abundance in CP-stars alpha<SUP>2</SUP>
  Canum Venaticorum, epsilon Ursae Majoris, Sirius and Vega.

---------------------------------------------------------
Title: Role of LDE-Type Flares in the GCR Modulation (1969-1972)
Authors: Antalová, A.; Rybák, J.; Kudela, K.; Venkatesan, D.
1995ICRC....4..530A    Altcode: 1995ICRC...24d.530A
  No abstract at ADS

---------------------------------------------------------
Title: E - W Distribution of Solar LDE - Type Flares and Galactic
    Cosmic
Authors: Jakimiec, M.; Storini, M.; Antalová, A.
1995ICRC....4..852J    Altcode: 1995ICRC...24d.852J
  No abstract at ADS

---------------------------------------------------------
Title: Periodicities of the LDE-type flare occurence (1969-1992)
Authors: Antalova, A.
1994AdSpR..14j.721A    Altcode: 1994AdSpR..14..721A
  The power spectrum was calculated for the time series of the LDE-type
  flare occurence during the last three solar cycles (the 20-th, the
  21-st and the first part of the 22-nd cycle). LDE-type flares (Long
  Duration Events in SXR) are associated with the interplanetary protons
  (SEP and STIP as well), energized coronal archs and radio type IV
  emission. Generally, in all the cycles considered, LDE-type flares
  mainly originated during a 6-year interval of the respective cycle
  (2 years before and 4 years after the sunspot cycle maximum). The
  following significant periodicities were found: <P />in the 20-th cycle:
  1.4, 2.1, 2.9, 4.0, 10.7 and 54.2 of month, <P />in the 21-st cycle:
  1.2, 1.6, 2.8 4.9, 7.8 and 44.5 of month, <P />in the 22-nd cycle,
  till March 1992: 1.4, 1.8, 2.4, 7.2, 8.7, 11.8 and 29.1 of month,
  <P />in all interval (1969-1992): <P />1. the longer periodicities:
  232.1, 121.1 (the dominant at 10.1 of year), 80.7, 61.9 and 25.6
  of month, <P />2. the shorter periodicities: 4.7, 5.0, 6.8, 7.9,
  9.1, 15.8 and 20.4 of month.. Solar variability has an extremely
  complex time dependence. The Sun is a multiperiodic system. The strong
  periodicities “near 155 and 270 days” were found also in the LDE-type
  flare occurence.

---------------------------------------------------------
Title: Cosmic-Ray Modulation and Long-Duration Solar Flare Events
Authors: Kudela, K.; Antalova, A.; Venkatesan, D.; Rybak, J.
1994SoPh..154..371K    Altcode:
  The correlation between the long-term intensity variations of cosmic
  rays at neutron monitor energies and the LDE index measure of solar
  flares with long-lasting soft X-ray emissions is reported. Three
  subsequent solar cycles, 20-22, are taken into account and half-monthly
  data are analyzed. Possible explanation of this correlation is discussed
  in terms of the recent concepts of cosmic-ray modulation, in particular
  with merged interaction regions affecting the cosmic-ray intensity.

---------------------------------------------------------
Title: The magnetic reversal of the Sun and manifestations of solar
    activity
Authors: Antalova, A.
1994CoSka..24...19A    Altcode:
  The affinity of the LDE-type flare locations to the reversed coronal
  magnetic sectors (and their boundaries) is studied. The Sun's gradual
  magnetic reversal (as described by computed coronal field structures)
  is compared with the occurrence of a flare activity in the solar
  unipolar coronal magnetic sectors. It is shown that the active regions
  of the 21st and 22nd cycles, giving rise to the LDE-type flares,
  are concentrated in the sectors of reversed magnetic polarity.

---------------------------------------------------------
Title: Catalogue of LDE-type flares (1992-1993)
Authors: Antalova, A.
1994CoSkS..24..137A    Altcode:
  The continuation of the list of long-lasting SXR flares (LDE-type)
  is given in a computer-file form. The latter contains the list of
  LDE flares observed from June 1992 to June 1993, and ties in timewise
  with the previous papers. The LDE-type flare occurence (of C, M and
  X- SXR classes) on the whole solar disk (D) and in the northern (N)
  and southern (S) hemispheres, respectively, are given in Table 2.

---------------------------------------------------------
Title: Catalogue of LDE-type flares (1992 - 1993).
Authors: Antalová, A.
1994CoSka..24..137A    Altcode:
  No abstract at ADS

---------------------------------------------------------
Title: Coronal Holes and the Locations of the LDE-Type Flares
Authors: Antalova, A.
1994scs..conf..263A    Altcode: 1994IAUCo.144..263A
  A qualitative analysis is presented of a possible link between two
  physical processes on the Sun, namely the gradual magnetic reversal
  of the large-scale magnetic field of the Sun, and the increase of a
  flare activity in the solar sectors where the polarity reversal of
  the faint large-scale magnetic field is observed.

---------------------------------------------------------
Title: Long Duration Solar Flare Events and Cosmic Ray Modulation
    (1969-1992)
Authors: Antalova, A.; Kudela, K.; Venkatesan, D.; Rybak, J.
1994scs..conf..499A    Altcode: 1994IAUCo.144..499A
  The authors present the results of a correlation analysis between the
  galactic cosmic ray intensity decrease (as observed on Calgary neutron
  monitor station) and the occurrence of SXR long-lasting (LDE-type)
  solar flares represented by the LDE-type flare index FI. It is shown,
  that for the solar cycle with the lower monthly values of FI (the
  21-st solar cycle) the correlation coefficient is slighter (about 0.4)
  as compared to the cycles with the higher LDE-type flare activity
  (about 0.6, in the 20-th and the 22-nd cycles).

---------------------------------------------------------
Title: Flaring Loops and Flaring Arches
Authors: Antalová, A.
1994emsp.conf..197A    Altcode:
  No abstract at ADS

---------------------------------------------------------
Title: Fourier Analysis of the LDE-Type Flare Occurence (1969-1991)
Authors: Antalová, A.
1994step.conf..113A    Altcode:
  No abstract at ADS

---------------------------------------------------------
Title: The LDE-Type Flare Occurrence (1969-1993)
Authors: Antalova, A.
1994scs..conf..279A    Altcode: 1994IAUCo.144..279A
  The occurrence of long-duration events in SXR (LDE-type flares)
  in the last three cycles has been investigated. LDE-type flares are
  associated with the interplanetary protons, energized coronal archs
  and radio type IV emission. Significant periodicities found are listed.

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

---------------------------------------------------------
Title: Catalogue of LDE-type flares (1991-1992)
Authors: Antalova, A.
1993CoSkS..23..131A    Altcode:
  The continuation of the list of long-lasting SXR flares (LDE-type)
  from November 1991 to June 1992 is given in a computer-file form. The
  maximum values of the sunspot and H-alpha grouped solar flare numbers
  belong to the 21-st solar cycle (the second half of 1979). The 22-nd
  cycle displayed the highest CR decrease and LDE-type flare occurence
  of the last three solar cycles.

---------------------------------------------------------
Title: The Galactic Cosmic Ray Intensity Modulation Effects and the
    LDE-Type Solar Flare Occurence (1969-1991)
Authors: Antalová, A.; Kudela, K.; Venkatesan, D.; Rybák. J.
1993ICRC....3..579A    Altcode: 1993ICRC...23c.579A
  No abstract at ADS

---------------------------------------------------------
Title: Catalogue of LDE-type flares (1991 - 1992).
Authors: Antalová, A.
1993CoSka..23..131A    Altcode:
  No abstract at ADS

---------------------------------------------------------
Title: The Monthly Occurrence of LDE Flares (1969-1990)
Authors: Antalova, A.; Viktorinova, B.
1992sers.conf..431A    Altcode:
  No abstract at ADS

---------------------------------------------------------
Title: Catalogue of LDE-type flares (1990-1991)
Authors: Antalova, A.
1992CoSkS..22..227A    Altcode:
  The continuation of the list of long-lasting SXR flares (LDE-type)
  from May 1990 to October 1991 is given in a computer-file form. The
  LDE-type flare occurrence (of M and X-SXR classes) on the whole solar
  disk (D) and in the northern (N) and southern (S) hemispheres, is
  considered. The maximal monthly occurrence of LDE flares in January
  1989 (N(D)=68, N(S)=55) and March 1991 (N(D)=67, N(S)=62) belongs
  to the southern solar hemisphere. In March 1989 (N(D)=60, N(N)=52)
  the maximal northern occurrence was observed.

---------------------------------------------------------
Title: The Hα Development of an Intense Limb Flare and Associated
    Flaring Arches
Authors: Antalova, A.; Ogir, M. B.
1992SoPh..138..361A    Altcode:
  The Hα analysis of the development of the strong impulsive and faint
  gradual phase of the June 26, 1983 flare indicates the following:
  (1) The flare originated from two microprominences on the southeast
  border of NOAA 4227. Several similar events are summarized in Table
  II. (2) The main flare structure was a flare cone, which consisted
  of a bright surge-like stream, elevated above two flare ribbons
  (located in the cone's base). The flare cone had a height of about 40
  × 10<SUP>3</SUP> km and lasted 4 min in Hα. The upper part of the
  cone was terminated by a very fine loop, which was bent to the west,
  where later a chromospheric brightening occurred at the footpoint of
  a flaring arch. A 300 keV burst and radio spikes were observed during
  the maximum flare phase. (3) The flaring arch system, with its apex
  at a height of about 48 × 10<SUP>3</SUP> km, formed the skeleton for
  the coronal helmet structure (Figure 7(c)). The velocity of the plasma
  moving along the flaring arch was between 3500 km s<SUP>−1</SUP>}
  and 6900 km s<SUP>−1</SUP>} during the first brightening (14:07 UT).

---------------------------------------------------------
Title: Fourier Analysis of the LDE Flare Index (1969 - 1991)
Authors: Antalova, A.
1992ASPC...27..377A    Altcode: 1992socy.work..377A
  No abstract at ADS

---------------------------------------------------------
Title: Catalogue of LDE flares (1990 - 1991).
Authors: Antalová, A.
1992CoSka..22..227A    Altcode:
  No abstract at ADS

---------------------------------------------------------
Title: The Statistics of CA 11-K Plage Macrostructure (January 1969 -
    May 1980)
Authors: Antalova, A.; Stepanyan, N. N.
1992ASPC...27..256A    Altcode: 1992socy.work..256A
  No abstract at ADS

---------------------------------------------------------
Title: The Relation of the Sunspot Magnetic Field and Penumbra-umbra
    Radius Ratio
Authors: Antalova, A.
1991BAICz..42..316A    Altcode:
  Indirect proportionality between the sunspot magnetic field BL and
  penumbra-umbra radius ratio k is described. The observed functions BL =
  f(k) are given using the data from 74 regular sunspots, observed from
  1968 to 1976 and 15 regular sunspots observed in 1977. It is shown
  that the smaller value BL is observed in the regular sunspot with
  larger value k. This result is found to be in quantitative agreement
  with Saniga's alternative view of the sunspot phenomena (1990).

---------------------------------------------------------
Title: LDE Flares in the 21st Solar Cycle (1976-1986). 1. Comparison
    of the Time Occurrences of H-alpha and LDE Flares
Authors: Viktorinova, B.; Antalova, A.
1991BAICz..42..144V    Altcode:
  The temporal behavior of H-alpha grouped flares and LDE-type flares
  is examined to determine whether the LDE-types are more prevalent in
  certain phases of the solar cycle. A chronological account of solar
  activity is presented, and observational data are listed for flare
  characteristics. Mathematical analyses of annual and monthly flares
  are presented with attention given to the north-south asymmetry
  and significant short-term pulses of the LDE flares. The LDE (M-X)
  flare occurrence conforms to a parabola as does the 10.8-cm radio
  flux. Correlation of these parameters with the coronal density is
  considered, and it is noted that the higher number of LDE flares in
  the Northern Hemisphere is compensated by increased Southern Hemisphere
  activity in the decline phase.

---------------------------------------------------------
Title: The LDE Flares in the 20th Solar Cycle 1. Comparison of the
    Time Behaviour of H-alpha Grouped and LDE Flares
Authors: Antalova, A.; Viktorinova, B.
1991BAICz..42..133A    Altcode:
  The numerical series of H-alpha and LDE flares are tested and compared
  for the years 1969-1976, using methods of statistical analysis. The
  results show that the occurrence of H-alpha flares can be expressed by
  an exponential function. The analytical expression of the LDE (M - X)
  flare occurrence (their SXR duration exceeds 2 hours) is a parabola
  or a set of spline functions. Time intervals with increased flare
  activities were observed in the years 1970, 1972 and 1974, whereas
  decreased flare activity was found in 1971 and 1975.

---------------------------------------------------------
Title: Long-decay Soft X-ray Flares. 4. Contact Arcade 1B/X3 LDE
Flare 1982 June 4, 13:13 UT
Authors: Ogir, M. B.; Antalova, A.; Bendik, P.
1991BAICz..42...31O    Altcode:
  The H-alpha morphology of the June 4, 1982, 13:13 UT, 1B/X3 LDE flare
  was analyzed from early onset through the maximum to the declining
  phase of the flare. The flare has been classified as a C-type flare,
  but an A-type hot component is also present. In the course of the LDE
  flare, three dipolar arcades bridging H-alpha ribbons were observed
  to originate. The main arcade, Arc 1, was connected with an erupted
  penumbral filament pF2 and was above spots A and B, forming a delta
  configuration. The origination of Arc 3 and the intermittent Arc 2
  are not related to the erupted filament. All three arcades displayed a
  common negative ribbon S 1. The contact ribbon S 1 ran along the neutral
  line in the center of the delta configuration. A similar contact of two
  different flare loops in a common ribbon has been observed in several
  SMY flares. Therefore, a contact ribbon common to several flare arcades
  may be a general symptom of the development of extended flares.

---------------------------------------------------------
Title: Catalogue of LDE flares (1989 - 1990)
Authors: Antalova, A.
1991CoSka..21..205A    Altcode:
  The continuation (February 1989 - April 1990) of the list of
  geoeffective LDE flares is contained in Table 1. Table 2 gives new data
  on further LDE flares observed from April 1980 to 1985. The data in
  Table 2 refer to a) newly identified weak LDE flares of the SXR class
  C, b) new flares with SXR duration of 2 hours, c) supplemental data on
  some of the mightier LDE flares, published earlier. Table 3 gives the
  monthly, semiannual and yearly counts of LDE flares in cycle 22. In
  cycle 22 (Oct. 1986 - April 1990) there are 1277 (C-X) and 549 (M-X)
  class LDE flares.

---------------------------------------------------------
Title: Flare Spray 1982 June 4, 14:24 UT
Authors: Antalova, A.; Ogir, M. B.
1990BAICz..41..368A    Altcode:
  The H-alpha morphology of the white-light impulsive 1B/X2 flare
  of June 4, 1982, exhibits a pinch-effect signature in the form of
  a conical plasmoid H-alpha flare structure feature which grew in
  size at 200 km/sec along the cone's axis (from base to apex). The
  base of the emission cone was formed by two close ribbons. A narrow
  emission filament was located along the axis of the flare cone. The
  flare spray was generated as the final product of the flare cone's
  development; it 'gushed' from the top of the axial high-energy
  descending filament. After the generation of the flare spray, an abrupt
  decrease was observed in the flare cone's length as well as in its
  H-alpha intensity.

---------------------------------------------------------
Title: The gradual type SXR flares
Authors: Antalova, A.; Viktorinova, B.
1990AN....311..358A    Altcode:
  The temporal variations of the occurrence of the (M-X) LDE flares
  with the soft X-ray (SXR) duration exceeding 2 hours throughout the
  20th and the 21st cycles are considered. The characteristics of the
  20th cycle: the maximum value of the observed yearly number of LDE
  flares was in the 1970 (with the total 225 LDE flares observed). The
  increased LDE flare activities were observed in the years 1972 and
  1974. The characteristics of the 21st cycle: the large occurrence
  of the (M-X) LDE flares was observed from 1979 to 1982. The yearly
  numbers of the (M-X) LDE flares in 1980 (168), 1981 (151), and 1982
  (135) are comparable. The fast decrease of the whole flare activity
  began at 1983. The percentual representation of the (M-X) LDE flares
  in the occurrence rate of all H-alpha flares fluctuated between 1 and
  3 percent.

---------------------------------------------------------
Title: Catalogue of LDE flares (1988 - 1989)
Authors: Antalova, A.
1990CoSka..19...59A    Altcode:
  The continuation (July 1988 - January 1989) of the list of geoeffective
  LDE flares is contained in Table 1. Table 2 gives new data on further
  LDE flares observed from July 1972 to March 1980. The data in Table
  2 refer to a) newly identified weak LDE flares of the SXR class C, b)
  new flares with SXR duration of 2 hours, c) supplemental data on some
  of the mightier LDE flares, published earlier.

---------------------------------------------------------
Title: Monthly counts of LDE flares (January 1969 - March 1989)
Authors: Antalova, A.
1990CoSka..19..145A    Altcode:
  The monthly counts of LDE flares were determined from the Catalogue
  of LDE flares and its Supplements (Antalova 1987, 1988, 1989,
  1990). Tables 1 (cycle 20), 2 (cycle 21) and 3 (part of cycle 22)
  give the distribution of the observed numbers of LDE flares in terms of
  three parameters: a) SXR importance of LDE flares, b) overall duration
  of the SXR flare emission, c) location of the LDE flare in the northern
  or southern solar hemisphere. The LDE flare index is given in the last
  column of all tables. The arrangement of Table 4 (half-year numbers)
  and Table 5 (yearly numbers) is identical with one of the Tables 1 - 3.

---------------------------------------------------------
Title: Geometric Properties of Solar Flares and Their Energetics
Authors: Antalova, A.; Jakimiec, M.
1989BAICz..40..311A    Altcode:
  The mutual relationship of 18 geometrical and energy variables of
  404 flares has been considered. It was found that (1) approximatelly
  60 percent of the total variance of the system (x1 - x18) could be
  explained by 3 - 4 F(j) factors; (2) the lowest H-alpha loops of the
  flare arcade (x 13) have comparable mean dimensions for both studied
  flare groups (during the maximum H-alpha phase, the height of the lowest
  flare arcade loops is about 7000 km); (3) energetically significant
  'major flares' acquire larger lengths of the flare ribbons, as well as
  ranges and volumes of the supplemental flare structures, than impulsive
  flares; and (4) commonly held views about simple relationships between
  H-alpha or SXR flare importance and the flare duration are in error. A
  relationship was found between H-alpha duration and the comprehensive
  flare index.

---------------------------------------------------------
Title: Supplement to the catalogue of LDE flares (July 1986 - June
    1988) - - Part 2
Authors: Antalova, A.
1989CoSka..18...41A    Altcode:
  The continuation (July 1986 - June 1988) of the list of geoactive
  LDE solar flares is contained in Table 1. Table 2 gives new data on
  further flares observed in the analyzed period of solar cycles 20 and
  21 (January 1969 - June 1986). The data in Table 2 refer to a) newly
  identified weak LDE flares of the SXR class C, b) new flares with SXR
  duration of 2 hours, c) supplemental data on some of the mightier LDE
  flares, published earlier.

---------------------------------------------------------
Title: The Relation Between Hα and SXR Emission of the Flares
Authors: Antalova, A.
1989ESASP.285..145A    Altcode: 1989rsp..conf..145A
  The evolutionary coincidence between the occurrence of the LDE flares
  and the formation of the evolving delta configuration, in the solar
  active region, was found. Fifty-one cases of LDE flares were analyzed
  from the viewpoint of the precise location of their flare loop arcade
  (located above delta configuration). The quasi-delta configurations
  (i.e., kinematical joining of the two stable spots of the opposite
  magnetic induction) are not LDE flare productive.

---------------------------------------------------------
Title: Long-decay Soft X-ray Flares. 3. H-alpha Activity in the
    Interribon Space of the LDE Flares
Authors: Antalova, A.; Ogir, M. B.
1988BAICz..39...97A    Altcode:
  Twenty cases of LDE flares have been analyzed from the viewpoint of
  the development of their morphology in the H-alpha line. It has been
  found that LDE flares may be classed as: (1) 'one-ribbon' flares,
  in which the long-lasting H-alpha emission loops are arranged along
  the axis of the filament, or along its channel; (2) two-ribbon flares;
  and (3) three-ribbon flares which are a combination of the first two
  types. The system of central loops (SCL) of the three-ribbon flares,
  is situated along the axis of the interribbon space and is a dynamic
  formation which cannot be mistaken for flare-loop tops. The repeated
  energy release, which occurs in the lower part of the interribbon space,
  indicates that the accumulation of energy, required for the formation
  of SCL and also for the trigger mechanism of the flare is concentrated
  in the low structures (lower than 3.5-7.0 thousand kilometers).

---------------------------------------------------------
Title: Supplement of the catalogue of LDE (Long Duration Event)
    flares.
Authors: Antalová, A.
1988CoSka..17..301A    Altcode:
  No abstract at ADS

---------------------------------------------------------
Title: Book Review: The statistics of sunspots (Statistika
    pjatnoobrazovatelnoj dejatelnosti solntsa. / Nauka, Moscow, 1986.
Authors: Antalova, A.
1987SoPh..109..199A    Altcode:
  No abstract at ADS

---------------------------------------------------------
Title: Book Review: Third Asian-Pacific Regional Meeting of the
    IAU. (Reprinted from Astrophysics and Space Science, V. 118, no. 1/2;
    V. 119, no. 1 (1986)) / Reidel, 1986.
Authors: Dwivedi, B. N.; Antalová, A.; Dwivedi, B. N.
1987SoPh..109..199D    Altcode:
  No abstract at ADS

---------------------------------------------------------
Title: Catalogue of LDE flares (January 1969 - March 1986)
    differential rotation of the Sun during the period 1921-1971
Authors: Antalova, A.
1987CoSka..16...79A    Altcode:
  The catalogue of LDE flares contains data on 646 flares observed
  in the 20th and on 1029 flares observed in the 21st cycle of solar
  activity. LDE flares constitute an important subgroup of two-ribbon
  flares. They are characterized by a strong and long-lasting process of
  magnetic field reconnection, they produced accelerated protons which
  propagate into interplanetary space and generate SID's by enhanced
  shortwave emission.

---------------------------------------------------------
Title: Evolutionary aspects of the solar active regions.
Authors: Stepanian, N. N.; Antalova, A.
1987PAICz..66...47S    Altcode: 1987eram....1...47S
  The observational results of the two aspects of the evolution of active
  regions are considered: (1) the evolutionary changes indicated in the
  altitudinal distribution of temperature and density in active elements,
  (2) the relation of flares to local and large scale magnetic fields
  on the solar surface.

---------------------------------------------------------
Title: Long-Decay Soft X-Ray Flares, 2. Three-parallel-ribbon LDE
Flare, 1981 October 12, 06:15 UT
Authors: Ogir, M. B.; Antalova, A.
1986BAICz..37..344O    Altcode:
  Twenty-seven out of 106 solar flares that occurred in two closely spaced
  regions between October 7 and October 14, 1981 are analyzed with regard
  to H-alpha and soft- and hard-X-ray emissions. The H-alpha and X-ray
  analysis of the LDE (long-duration-event) flare of October 12, 1981 is
  presented. On October 12, three strong X-ray flares were seen at 04:38,
  06:15 and 10:33 UT. A detailed analysis of flare at 06.15 UT showed
  that the flare had two impulsive hard X-ray phases. In the course of the
  second impulsive phase, the dark post-flare loops vanished and the third
  central ribbon became more distinct. The third central H-alpha ribbon
  can be interpreted as radiation which is generated in the hot loop tops,
  although the loops were located in the bottom part of the arcade. It
  was proved that flare pairs had quasi-synchronous origins in four cases.

---------------------------------------------------------
Title: The duration of flares and their radio emission
Authors: Antalova, A.
1986BAICz..37..107A    Altcode:
  The means durations of 906 H-alpha flares were calculated as a
  function of their radio, X-ray, and areal characteristics, and a
  similar calculation was performed for the durations of 215 soft X-ray
  flares. It was found that H-alpha flares associated only with type
  II radio bursts have, on the average, shorter durations than flares
  associated with type IV radio emissions. The duration of the soft X-ray
  flares is related to a much hotter plasma, probably located in the
  geometrically higher layers of the flare as compared with the H-alpha
  flares. The soft flares associated only with type II radio bursts
  have an average duration smaller than that of flares associated with a
  type IV radio emission. The group of flares associated with type III
  radio bursts can be considered as a standard case of thermal flares,
  have a mean duration which does not depend on flare area. The mean
  duration is 40 minutes for M-flares and 60 minutes for X-flares.

---------------------------------------------------------
Title: The Duration of Flares and Their Radio Emission
Authors: Antalová, A.
1986BAICz..37..108A    Altcode:
  No abstract at ADS

---------------------------------------------------------
Title: The latitudinal distribution of sunspot area and variations
    of the differential rotation of the Sun during the period 1921-1971
Authors: Antalova, A.
1986CoSka..14..121A    Altcode:
  The distribution of the sunspot area is compared with the distribution
  of variations of the differential rotation in solar activity
  cycles Nos. 16 - 20 using butterfly diagrams. The variations of
  the differential angular rotation of the Sun for a particular year
  and latitude zone are defined as the difference between the average
  annual value of the daily sidereal angular rotation of sunspots and
  the average long-term (1921- 1982) value of the same quantity. Gilman
  et al. (1984) published the basic observation material related to
  the differential rotation. The analysis indicates that the zones
  on the Sun in which there is a large accumulation of sunspot areas
  display a smaller velocity than the long- term average zonal velocity
  (Tab. 3). The cases with faster rotation have an average annual value of
  the zonal sunspot area equal to 32000 millionths of the Sun's visible
  hemisphere (areal unit). The cases with slow rotation have an average
  annual value of the zonal area equal to 55000 units.

---------------------------------------------------------
Title: The rate of areal decrease of long-lived sunspots
Authors: Antalova, A.; Macura, R.
1986CoSka..14..163A    Altcode:
  The analysis of 30 long-lived “naked” sunspots, observed in the
  years 1969 -1976 (Tab. 1), and of 30 sunspots of the Zurich H-type,
  observed during the same period (Tab. 2), yielded the following results:
  1. Long-lived “naked” sunspots occur in all size categories ranging
  from small (U = 20 millionths of the visible solar hemisphere) to large
  sunspots (U = 110 millionths of the visible solar hemisphere). The
  Zurich H-type sunspots were of medium size (shown in Figs 4-6). Both
  groups of sunspots represent the final stage of the evolution of an
  active region. These sunspots are unipolar and have the same magnetic
  polarity as their neighbourhood. 2. The rate of decrease of the area
  of umbras of long-lived “naked” sunspots per day can be expressed
  by Eq (1), for the Zurich H-type sunspots by Eq (3). Linear relations
  of the decrease of areas of whole sunspots W were determined for
  both groups of sunspots and are expressed by Eqs (2) and (4). They
  indicate that the larger the initial area U$<SUB>o</SUB>$ of the
  sunspot, the larger the absolute value of the daily areal decrease
  of the sunspot. 3. The average daily relative rate of decay of the
  “naked” sunspots amounts to two hundredths of their initial area
  (Fig. 3). The average daily relative rate of areal decrease of the
  Zurich H-type sunspots is equal to two tenths of the area of the initial
  umbra (Fig. 6). The rate of decay of old unipolar sunspots, assuming
  they have the same area, depends on another parameters which can so
  far only be evaluated qualitatively. This parameter is the intensity
  of the sunspot's interaction with its ambient medium. The interaction
  mechanism is still not clear, but the “naked” sunspots form a group
  with an extremely low interaction intensity (Fig. 7).

---------------------------------------------------------
Title: Regional consultation on solar physics
Authors: Antalova, A.
1986rcsp.conf.....A    Altcode:
  No abstract at ADS

---------------------------------------------------------
Title: Proceedings of the 12th Regional Consultation on Solar Physics,
    held at Smolenice, Czechoslovakia, 19 - 24 May 1986.
Authors: Antalová, A.; Kopecký, M.; Hrivňák, I.; Sýkora, J.
1986csp..book.....A    Altcode:
  No abstract at ADS

---------------------------------------------------------
Title: Flare activity of regions with magnetic delta configuration
Authors: Antalová, A.
1986CoSka..15..281A    Altcode:
  The flares observed above the delta configuration are more energetic,
  compared to other flares of the same region. The unknown trigger
  mechanism of flares does not depend on the delta configuration. The
  flare activity of the certain delta configuration is variable and
  is mainly a function of energy supply (kinetic and magnetic) and of
  processes of accumulation and release of energy. In addition to the
  flares observed in expected sites of the four analysed regions (the
  place of an emerging new flux) there are some flares in unpreferred
  places. These flares probably resulted from relaxation process of the
  whole region.

---------------------------------------------------------
Title: Hα Solar Flare Activity in Bou 2030 and 2032, SERF Interval,
    October 6-8, 1979
Authors: Antalová, A.; Bendik, P.; Petrášek, J.
1985BAICz..36..347A    Altcode:
  During the SERF interval of the SMY, October 4 to 9, 1979, observations
  of regions Bou 2030 and 2032 were coordinated. The analysis of H-alpha
  observations indicates that, contrary to expectations, flares initiated
  in magnetically simple sunspot groups. The enhanced occurrence of
  flares was located in an area with pronounced changes of polarity and
  structure of the background field. In analysing the pre-flare situation
  in a particular active region, therefore, it is necessary to know the
  characteristics of the large-scale field as well.

---------------------------------------------------------
Title: Coincidence in subflare onsets in the October 1979 complex
    of activity
Authors: Antalova, A.
1985CoSka..13..157A    Altcode:
  In the October 1979 activity complex, the coincidences of the onsets
  of subflares, observed in various parts of the activity complex, were
  statistically proved to be real. The occurrence of subflare pairs from
  Bou 2030 and 2032, for which the subflare onset times differ by less
  than 5 minutes (Tab. 2) is statistically significant. The increased
  coincidence in the occurrence of subflare pairs, differing in onset by
  5 minutes or less, was not permanent. The coincidence was only observed
  on October 6 and 7, 1979 during the transit of the activity complex
  across the solar disk (SMY - SERF target). The result obtained for
  October 1979 activity complex agrees with the present idea of multiple
  energy release during the impulsive phase of solar flares.

---------------------------------------------------------
Title: Comprehensive solar flare indices and duration of H-alpha
    flares
Authors: Antalova, A.
1985CoSka..13..243A    Altcode:
  Table 1 gives the mean values of the duration of H-alpha flares as
  a function of their importance and subdivision by comprehensive
  flare index. The results were computed using data on 460 flares,
  observed in the years 1970-1974, and 561 flares, observed in the years
  1975-1979. The flare data were selected from extensive records of large
  flares, published by Dodson et al. (1975, 1980). Flares accompanied
  by a type IV radio burst produce electrons of higher velocities than
  flares accompanied by type II radio bursts. Table 1 indicates that the
  mean duration (D) of the same importance class of flares related to
  type II radio bursts is shorter and has a smaller standard deviation
  (S.D.) than the flares related to type IV radio bursts.

---------------------------------------------------------
Title: Long-Decay Soft X-Ray Flares. 1. Region McMath 11 926, June
    15, 1972
Authors: Antalová, A.; Ogir, M. B.
1984BAICz..35..276A    Altcode:
  The time-space occurrence and development of H-alpha flares, which were
  generated in McMath region 11926 on 15 June 1972, were analysed with
  regard to the activation of filaments and the development of filament
  channels. H-alpha films were obtained from the Crimean Astrophysical
  Observatory. The magnetic field of the studied region had the form of
  an S-field "island" surrounded by an extensive N-field.

---------------------------------------------------------
Title: Relationships of a growing magnetic flux region to flares
Authors: Martin, S. F.; Bentley, R. D.; Schadee, A.; Antalova, A.;
   Kucera, A.; Dezső, L.; Gesztelyi, L.; Harvey, K. L.; Jones, H.;
   Livi, S. H. B.; Wang, J.
1984AdSpR...4g..61M    Altcode: 1984AdSpR...4...61M
  Some sites for solar flares are known to develop where new magnetic
  flux emerges and becomes abutted against opposite polarity pre-existing
  magnetic flux (review by Galzauskas/1/). We have identified and analyzed
  the evolution of such flare sites at the boundaries of a major new and
  growing magnetic flux region within a complex of active regions, Hale
  No. 16918. This analysis was done as a part of a continuing study of the
  circumstances associated with flares in Hale Region 16918, which was
  designated as an FBS target during the interval 18 - 23 June 1980. We
  studied the initiation and development of both major and minor flares in
  Hα images in relation to the identified potential flare sites at the
  boundaries of the growing flux region and to the general development
  of the new flux. This study lead to our recognition of a spectrum of
  possible relationships of growing flux regions to flares as follows:
  (1) intimate interaction with adjacent old flux - flare sites centered
  at new/old flux boundary, (2) forced or “intimidated” interaction
  in which new flux pushes old field having lower flux density towards a
  neighboring old polarity inversion line where a flare then takes place,
  (3) “influential” interaction - magnetic lines of force over an old
  polarity inversion line, typically containing a filament, reconnect to
  the new emerging flux; a flare occurs with erupting filament when the
  magnetic field overlying the filament becomes too weak to prevent its
  eruption, (4) inconsequential interaction - new flux region is too small
  or has wrong orientation for creating flare conditions, (5) incidental -
  flare occurs without any significant relationship to new flux regions.

---------------------------------------------------------
Title: The Motions of the Umbras in Hale Active Regions 16 862 and
    16 863
Authors: Antalova, A.
1983BAICz..34...96A    Altcode:
  Observations of the umbral rotation motions of the leading spot
  of Hale AR 16 863 and the umbras of the main spots of 16 862 are
  presented. Substantial changes of the orientation of the geometrical
  axis of the umbra of the AR 16 863 was observed during May 22-24,
  1980. The average angular velocity was -1.8 deg/hr. The axes of both
  main umbras of AR 16 862 also rotated after May 24, 1980. These spots
  were preferred locations of the umbral subflares. The onset times of
  umbral rotation coincided with the appearance of new sunspots observed
  in the vicinity of the studied spots.

---------------------------------------------------------
Title: Observatory Skalnaté Pleso.
Authors: Sýkora, J.; Svoreň, J.; Antalová, A.
1983Kozmo..14..145S    Altcode:
  No abstract at ADS

---------------------------------------------------------
Title: Latitudinal distribution of sunspot areas during the period
    1874-1976
Authors: Antalova, A.; Gnevyshev, M. N.
1983CoSka..11...63A    Altcode:
  The distribution of sunspot areas in heliographic latitude has
  been analyzed, from the 12th to the 20th cycle, using Greenwich
  Observations. The resulting six-month sunspot area values of the
  latitudinal distribution are given for each 11-year cycle in tabular
  form and they are also plotted as contours in Figs 1 through 9. Within
  the solar cycles, there are numerous time variations, pulses of
  activity, which clearly show that the activity in certain latitudinal
  intervals is higher than in other heliographic latitudes. The width
  of these pulses is some tens of degrees in latitude and the duration
  from one half to two years. The times at which the pulses appear
  in both hemisphere do not coincide. There is no steady equatorward
  progression of a single maximum of activity throughout a given cycle,
  but the eleven-year cycle consists of the superposition of two or more
  pulses, which peak at different times and at different latitudes.

---------------------------------------------------------
Title: The photospheric Doppler shift observed in Hale ARs 16862
    and 16863 (May 22 and 23, 1980).
Authors: Antalová, A.
1983PDHO....5...93A    Altcode: 1984PDHO....5...93A
  A detailed spatial structure analysis of four Meudon photoelectric
  charts of the photospheric Doppler shift (magneto-sensitive line Fe
  I 630.25 nm) was done for Hale ARs 16862 and 16863 on May 22 and 23,
  1980. At the very beginning of the appearance of the new sunspots,
  temporary (lasting only a few hours), small dimensional, upward,
  photospheric motions, with an amplitude larger than 900 m s<SUP>-1</SUP>
  were observed. The result is valid for small new sunspots, which
  appeared in the penumbras of the large spots (16863p and 16862f). The
  umbra of the 16863p spot had complex velocity and structural patterns
  from May 21 to 23.

---------------------------------------------------------
Title: Emerging magnetic flux, flares and filaments - FBS interval
    16-23 June 1980
Authors: Martin, S. F.; Dezso, L.; Antalova, A.; Kucera, A.; Harvey,
   K. L.
1982AdSpR...2k..39M    Altcode: 1982AdSpR...2...39M
  17 emerging magnetic flux regions with arch filaments related to
  new sunspots were identified in Hale Active Region No. 16918 during
  the 7 day interval from 16-22 June. Most of the new flux regions
  were clustered around the filament channel between the old opposite
  polarity fields as were most of the flares. The two largest regions of
  new magnetic flux and a few of the smaller flux regions developed very
  near the end points of filaments. This suggests that the emergence of
  flux in existing active regions might be non-random in position along
  a filament channel as well as in distance from a filament channel. <P
  />We have analyzed the positions of 88 flares to date during about
  half of each day. We find that slightly more than half (50%) of the
  flares, irrespective of their size, are centered within the new flux
  regions. About 1/5 (20%) were centered on the border between the new
  flux and the adjacent older magnetic field. Less than 1/3 occurred
  outside of the newly emerging flux regions but in many cases were very
  close to the newly emerging flux. We conclude that at least 2/3 of
  the flares are intimately related to the emerging flux regions while
  the remaining 1/3 might be either indirectly related or unrelated to
  the emerging flux.

---------------------------------------------------------
Title: Studies of the Carina Nebula : IV. A new determination of
    the distances of the open clusters Tr 14, Tr 15 and Cr 228 based on
    Walraven Photometry.
Authors: The, P. S.; Bakker, R.; Antalova, A.
1980A&AS...41...93T    Altcode:
  The Walraven photometer attached to the 90 cm lightcollector of the
  Leiden Southern Station, Hartbeespoortdam (South Africa) has been
  used in 1974, 1975 and 1976 to study interesting objects located in
  the region of the Carina Nebula (NGC 3372). In this paper the results
  (see table XII) of the determination of the distances of the open
  clusters Tr 14, Tr 15, Tr 16 and Cr 228, most probably embedded in
  the Carina Nebula, is presented.

---------------------------------------------------------
Title: Galactic supernovae.
Authors: Antalová, A.
1979Kozmo..10....3A    Altcode:
  No abstract at ADS

---------------------------------------------------------
Title: Interstellar absorption in the region of Ass Scorpius OB 4.
Authors: Antalová, A.; Graham, J. A.
1978rscc.conf...19A    Altcode:
  No abstract at ADS

---------------------------------------------------------
Title: Interstellar Absorption in the Region of ASS-SCORPIUS-OB-4
Authors: Antalova, A.; Graham, J. A.
1977stcl.symp...19A    Altcode:
  No abstract at ADS

---------------------------------------------------------
Title: Interstellar matter and the evolution of stars.
Authors: Antalová, A.
1977Kozmo...8..106A    Altcode:
  No abstract at ADS

---------------------------------------------------------
Title: Interstellar Absorption in the Region of Ass Scorpius OB 4
Authors: Antalova, A.; Graham, J. A.
1976BAICz..27..193A    Altcode:
  VBLU photoelectric photometry is used to determine the interstellar
  absorption, photometric distances, and spectral types of 191 stars
  in the neighborhood of the Sco OB4 association. It is found that
  interstellar absorption in this region is extremely variable, with 55
  stars belonging to the association showing low absorption in comparison
  with stars located near a cold dark cloud south of the association. The
  mean distance of the OB stars in the association is estimated to be 1.6
  kpc, and it is suggested that the association may be only a part of a
  large complex of early-type stars extending from the H II region NGC
  6334 through the H II region NGC 6357 to the H II region NGC 6383. It
  is concluded that the present association and H II regions are situated
  at the distance of the first inner galactic arm.

---------------------------------------------------------
Title: UBV photographic photometry of stars in the
region AR<SUB>1950</SUB> : 17<SUP>h</SUP>03<SUP>m</SUP> -
17<SUP>h</SUP>41<SUP>m</SUP> Decl<SUB>1950</SUB> : -28.8° to -33.4°
Authors: Antalová, A.
1976CoSka...7..155A    Altcode:
  No abstract at ADS

---------------------------------------------------------
Title: UBV photographic photometry of stars in the
region AR<SUB>1950</SUB>: 17<SUP>h</SUP>03<SUP>m</SUP> -
17<SUP>h</SUP>41<SUP>m</SUP>, Decl<SUB>1950</SUB>: -28.8° to
    -33.4°. III. The catalogue and identification maps of open star
clusters: NGC 6405, NGC 6383, "NGC 6374", AV 2, NGC 6416 and
H<SUB>α</SUB> emissions region: GUM 67(Av 3), GUM 68 (Av 2)
Authors: Antalová, A.
1972BAICz..23..126A    Altcode:
  No abstract at ADS

---------------------------------------------------------
Title: UBV photographic photometry in the region AR<SUB>1950</SUB>:
    17<SUP>h</SUP>03<SUP>m</SUP> - 17<SUP>h</SUP>41<SUP>m</SUP>
Decl<SUB>1950</SUB>: -28.8° to -33.4°. II. Open star cluster TR
    28. Catalogue of 76 stars and identification map
Authors: Antalová, A.
1971BAICz..22...42A    Altcode:
  No abstract at ADS

---------------------------------------------------------
Title: The ratio of penumbral and umbral areas of sun-spots in the
    11-year solar activity cycle
Authors: Antalová, A.
1971BAICz..22..352A    Altcode:
  No abstract at ADS

---------------------------------------------------------
Title: UBV photographic photometry of stars in the
    region AR<SUB>1950</SUB> 17<SUP>h</SUP>03<SUP>m</SUP> -
17<SUP>h</SUP>41<SUP>m</SUP> Decl<SUB>1950</SUB>:-28.8° -
    33.4°. I. The catalogue and identification maps of 250 OB and 101
    photometrically interesting stars
Authors: Antalová, A.
1970BAICz..21..331A    Altcode:
  No abstract at ADS

---------------------------------------------------------
Title: Shape and evolution of photospheric regions with radiobursts
    IV flares
Authors: Antalová, A.
1969csph.conf...21A    Altcode:
  No abstract at ADS

---------------------------------------------------------
Title: The photospheric situation connected with the development of
    flares accompanied by the type IV radio bursts
Authors: Antalová, A.
1967BAICz..18...61A    Altcode:
  No abstract at ADS

---------------------------------------------------------
Title: Principal Characteristics of the 11-Year Solar Activity Cycle
Authors: Antalova, A.; Gnevyshev, M. N.
1965SvA.....9..198A    Altcode:
  No abstract at ADS

---------------------------------------------------------
Title: Interdependence of sunspot proper-motions and chromospheric
    flares
Authors: Antalová, A.
1965BAICz..16...32A    Altcode:
  No abstract at ADS

---------------------------------------------------------
Title: Principal Characteristics of the 11-Year Solar Activity Cycle
Authors: Antalova, A.; Gnevyshev, M. N.
1965AZh....42..253A    Altcode:
  No abstract at ADS

---------------------------------------------------------
Title: Proper motions of H- and J-type sunspots
Authors: Antalová, A.
1963BAICz..14...97A    Altcode:
  No abstract at ADS

---------------------------------------------------------
Title: Observations of Pluto in 1960
Authors: Antalová, A.; Antal, M.
1962BAICz..13...26A    Altcode:
  No abstract at ADS

---------------------------------------------------------
Title: Photometric parameters of Comet Burnham 1959k
Authors: Antalová, A.; Antal, M.
1961BAICz..12...71A    Altcode:
  No abstract at ADS

---------------------------------------------------------
Title: Notes on the proper motions of late-type sunspots
Authors: Antalová, A.
1961BAICz..12..108A    Altcode:
  No abstract at ADS

---------------------------------------------------------
Title: The observations of Pluto in 1959
Authors: Antalová, A.; Antal, M.
1960BAICz..11..231A    Altcode:
  No abstract at ADS