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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.
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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.
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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.
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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.
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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.
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Title: The Duration of Flares and Their Radio Emission
Authors: Antalová, A.
1986BAICz..37..108A Altcode:
No abstract at ADS
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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.
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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).
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Title: Regional consultation on solar physics
Authors: Antalova, A.
1986rcsp.conf.....A Altcode:
No abstract at ADS
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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
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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.
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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.
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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.
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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.
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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.
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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.
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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.
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Title: Observatory Skalnaté Pleso.
Authors: Sýkora, J.; Svoreň, J.; Antalová, A.
1983Kozmo..14..145S Altcode:
No abstract at ADS
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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.
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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.
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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
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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
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Title: Proper motions of H- and J-type sunspots
Authors: Antalová, A.
1963BAICz..14...97A Altcode:
No abstract at ADS
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Title: Observations of Pluto in 1960
Authors: Antalová, A.; Antal, M.
1962BAICz..13...26A Altcode:
No abstract at ADS
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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