Author name code: antalova ADS astronomy entries on 2022-09-14 author:"Antalova, Anna" ------------------------------------------------------------------------ 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. Bibcode: 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. Title: Time Evolution of low-Frequency Periodicities in Cosmic ray Intensity Authors: Kudela, K.; Rybák, J.; Antalová, A.; Storini, M. Bibcode: 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. Title: Comparing wavelet and traditional studies in the Gnevyshev Gap context Authors: Storini, M.; Laurenza, M.; Rybak, J.; Antalova, A.; Kudela, K. Bibcode: 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. Title: On the quasi-biennial modulation of galactic cosmic rays Authors: Storini, M.; Rybak, J.; Antalova, A.; Kudela, K. Bibcode: 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. Title: On the wavelet approach to cosmic ray variability Authors: Kudela, K.; Storini, M.; Antalova, A.; Rybák, J. Bibcode: 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. Title: The Solar and Cosmic-Ray Synodic Periodicity (1969 1998) Authors: Antalová, A.; Kudela, K.; Rybák, J. Bibcode: 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). Title: The Wavelet Analysis of the Solar and Cosmic-Ray Data Authors: Rybák, J.; Antalová, A.; Storini, M. Bibcode: 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). Title: Daily soft X-ray flare indices (1985 and 1986) Authors: Antalova, A. Bibcode: 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. Title: Cosmic ray/Soft X-ray background relationship from July 1968 to June 1987 Authors: Jakimiec, M.; Antalova, A.; Storini, M. Bibcode: 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. Title: Daily soft X-ray flare indices (1983 and 1984). Authors: Antalová, A. Bibcode: 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. Title: Daily soft X-ray flare indices (1983 and 1984) Authors: Antalova, A. Bibcode: 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. 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. Bibcode: 2000ESASP.463..403O Altcode: 2000sctc.proc..403O No abstract at ADS Title: Variability of the CR/XBG-L Relationship during the Solar Cycle Evolution Authors: Jakimiec, M.; Antalova, Anna; Storini, Marisa Bibcode: 2000ESASP.463..337J Altcode: 2000sctc.proc..337J No abstract at ADS Title: The Variations of the Solar Activity and the Low Rigidity Cosmic Rays (1969-1998) Authors: Antalová, A.; Kudela, Karel; Rybak, Jan Bibcode: 2000ESASP.463..281A Altcode: 2000sctc.proc..281A No abstract at ADS Title: The Intermittency of the Solar Intermediate-Term Periodicity (1969-1998) Authors: Rybák, J.; Antalova, Anna; Storini, Marisa Bibcode: 2000ESASP.463..419R Altcode: 2000sctc.proc..419R No abstract at ADS Title: Synodic Recurrency of Cosmic Rays Authors: Antalová, A.; Kudela, K.; Langer, R. Bibcode: 1999ESASP.448.1125A Altcode: 1999ESPM....9.1125A; 1999mfsp.conf.1125A No abstract at ADS Title: Fourier Analysis of the LDE-type Flare Occurrence (1969 - 1997) Authors: Antalová, A. Bibcode: 1999ESASP.448..743A Altcode: 1999ESPM....9..743A; 1999mfsp.conf..743A No abstract at ADS Title: Cosmic-ray intensity versus solar soft X-ray background in cross-correlation analysis Authors: Jakimiec, Maria; Antalová, Anna; Storini, Marisa Bibcode: 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). Title: Soft X-ray flare indices in 1981 and 1982 years Authors: Antalova, A. Bibcode: 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. Title: Daily soft X-ray flare indices (1979 and 1980) Authors: Antalova, A. Bibcode: 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). Title: Daily soft X-ray flare indices (1979 and 1980). Authors: Antalová, A. Bibcode: 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. Title: On the double-peaked cycle of solar activity: a connection with the heliomagnetic field. Authors: Storini, M.; Feminella, F.; Antalová, A.; Massetti, S. Bibcode: 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. Title: Lomnický Štít and Calgary cosmic ray measurments during the 22-nd solar cycle. Authors: Antalová, A.; Kudela, K.; Langer, R. Bibcode: 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. Title: LDE-type events in solar soft X-rays (1986 year). Authors: Antalová, A. Bibcode: 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. Title: Coronal mass ejections, flares, and geomagnetic storms Authors: Landi, R.; Moreno, G.; Storini, M.; Antalová, A. Bibcode: 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. Title: 1977 and 1978 daily soft X-ray flare indices Authors: Antalova, A. Bibcode: 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). Title: 1977 and 1978 daily soft X-ray flare indices. Authors: Antalová, A. Bibcode: 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. Title: The LDE flares (1969-1990) Authors: Antalová, A.; Viktorínová, B. Bibcode: 1998PAICz..88...75A Altcode: No abstract at ADS Title: June 26, 1983, 14:07 UT 300 keV, 3B/M7 east-limb solar flare Authors: Antalová, A.; Ogir, M. B. Bibcode: 1998PAICz..88...71A Altcode: No abstract at ADS Title: Spatial and temporal distribution of the LDE-type flares. Authors: Antalová, A. Bibcode: 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. Title: On Time Lags Between Soft X-ray Flares and Galactic CR Modulation (1969-1976) Authors: Antalová, A.; Jakimiec, M.; Storini, M. Bibcode: 1998asct.conf..475A Altcode: No abstract at ADS Title: 22nd Cycle's Sectorial Distribution of LDE-type Flaring Centers Authors: Antalová, A. Bibcode: 1998asct.conf..117A Altcode: No abstract at ADS Title: Solar soft X-ray parameters: 1969-1976 autocorrelation functions Authors: Jakimiec, M.; Storini, M.; Antalova, A. Bibcode: 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. Title: The 20-th solar cycle minimum and its daily soft X-ray flare index (1975-1976) Authors: Antalova, A. Bibcode: 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). Title: The 20th solar cycle minimum and its daily soft X-ray flare index (1975 - 1976). Authors: Antalová, A. Bibcode: 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. Bibcode: 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. Title: Multivariate daily sequence analyses of GCR/solar X-ray parameters Authors: Jakimiec, M.; Storini, M.; Antalová, A. Bibcode: 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. Title: To Forecast Huge Forbush Decreases During Solar Activity Cycles Authors: Storini, M.; Massetti, S.; Antalova, A. Bibcode: 1997ICRC....1..409S Altcode: 1997ICRC...25a.409S No abstract at ADS Title: Daily soft X-ray flare index (1969-1972) Authors: Antalova, A. Bibcode: 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. Bibcode: 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). Title: Long Duration Soft X-ray Events and Galactic Cosmic Ray Modulation Authors: Antalova, A.; Rybak, J.; Kudela, K.; Venkatesan, D. Bibcode: 1996ASPC...95..119A Altcode: 1996sdit.conf..119A No abstract at ADS Title: Magnetic Reversal in the 22nd Solar Cycle and Spatial Distribution of LDE-type Flares Authors: Antalova, A.; Jakimiec, M. Bibcode: 1996ASPC...95...82A Altcode: 1996sdit.conf...82A No abstract at ADS Title: Catalogue of LDE-type flares (1994 - 1995). Authors: Antalová, A. Bibcode: 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. 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. Bibcode: 1996ASPC...95..437A Altcode: 1996sdit.conf..437A No abstract at ADS Title: LDE-type flares and heliosphere (1969 - 1995). Authors: Antalová, A. Bibcode: 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. Title: Solar neutron measurements on the Solar Probe Authors: Kudela, K.; Kuznetsov, S. N.; Antalová, A. Bibcode: 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. Bibcode: 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. Bibcode: 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. Bibcode: 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. Bibcode: 1995ICRC....4..534A Altcode: 1995ICRC...24d.534A No abstract at ADS Title: Sectorial Distribution of LDE-Type Flares Authors: Antalová, A.; Jakimiec, M. Bibcode: 1995ICRC....4...70A Altcode: 1995ICRC...24d..70A No abstract at ADS Title: Catalogue of LDE-type flares (1993 - 1994). Authors: Antalová, A. Bibcode: 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. Bibcode: 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. Bibcode: 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 Bibcode: 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 alpha2 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. Bibcode: 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. Bibcode: 1995ICRC....4..852J Altcode: 1995ICRC...24d.852J No abstract at ADS Title: Periodicities of the LDE-type flare occurence (1969-1992) Authors: Antalova, A. Bibcode: 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:

in the 20-th cycle: 1.4, 2.1, 2.9, 4.0, 10.7 and 54.2 of month,

in the 21-st cycle: 1.2, 1.6, 2.8 4.9, 7.8 and 44.5 of month,

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,

in all interval (1969-1992):

1. the longer periodicities: 232.1, 121.1 (the dominant at 10.1 of year), 80.7, 61.9 and 25.6 of month,

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. Bibcode: 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. Bibcode: 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. Bibcode: 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. Bibcode: 1994CoSka..24..137A Altcode: No abstract at ADS Title: Coronal Holes and the Locations of the LDE-Type Flares Authors: Antalova, A. Bibcode: 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. Bibcode: 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. Bibcode: 1994emsp.conf..197A Altcode: No abstract at ADS Title: Fourier Analysis of the LDE-Type Flare Occurence (1969-1991) Authors: Antalová, A. Bibcode: 1994step.conf..113A Altcode: No abstract at ADS Title: The LDE-Type Flare Occurrence (1969-1993) Authors: Antalova, A. Bibcode: 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. Bibcode: 1994step.conf..151K Altcode: No abstract at ADS Title: Catalogue of LDE-type flares (1991-1992) Authors: Antalova, A. Bibcode: 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. Bibcode: 1993ICRC....3..579A Altcode: 1993ICRC...23c.579A No abstract at ADS Title: Catalogue of LDE-type flares (1991 - 1992). Authors: Antalová, A. Bibcode: 1993CoSka..23..131A Altcode: No abstract at ADS Title: The Monthly Occurrence of LDE Flares (1969-1990) Authors: Antalova, A.; Viktorinova, B. Bibcode: 1992sers.conf..431A Altcode: No abstract at ADS Title: Catalogue of LDE-type flares (1990-1991) Authors: Antalova, A. Bibcode: 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. Bibcode: 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 × 103 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 × 103 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−1} and 6900 km s−1} during the first brightening (14:07 UT). Title: Fourier Analysis of the LDE Flare Index (1969 - 1991) Authors: Antalova, A. Bibcode: 1992ASPC...27..377A Altcode: 1992socy.work..377A No abstract at ADS Title: Catalogue of LDE flares (1990 - 1991). Authors: Antalová, A. Bibcode: 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. Bibcode: 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. Bibcode: 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. Bibcode: 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. Bibcode: 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. Bibcode: 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. Bibcode: 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. Bibcode: 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. Bibcode: 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. Bibcode: 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. Bibcode: 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. Bibcode: 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. Bibcode: 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. Bibcode: 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. Bibcode: 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. Bibcode: 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. Bibcode: 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. Bibcode: 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. Bibcode: 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. Bibcode: 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. Bibcode: 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. Bibcode: 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. Bibcode: 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. Bibcode: 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. Bibcode: 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$o$ 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. Bibcode: 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. Bibcode: 1986csp..book.....A Altcode: No abstract at ADS Title: Flare activity of regions with magnetic delta configuration Authors: Antalová, A. Bibcode: 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. Bibcode: 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. Bibcode: 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. Bibcode: 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. Bibcode: 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. Bibcode: 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. Bibcode: 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. Bibcode: 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. Bibcode: 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. Bibcode: 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-1 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. Bibcode: 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.

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. Bibcode: 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. Bibcode: 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. Bibcode: 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. Bibcode: 1977stcl.symp...19A Altcode: No abstract at ADS Title: Interstellar matter and the evolution of stars. Authors: Antalová, A. Bibcode: 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. Bibcode: 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 AR1950 : 17h03m - 17h41m Decl1950 : -28.8° to -33.4° Authors: Antalová, A. Bibcode: 1976CoSka...7..155A Altcode: No abstract at ADS Title: UBV photographic photometry of stars in the region AR1950: 17h03m - 17h41m, Decl1950: -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 Hα emissions region: GUM 67(Av 3), GUM 68 (Av 2) Authors: Antalová, A. Bibcode: 1972BAICz..23..126A Altcode: No abstract at ADS Title: UBV photographic photometry in the region AR1950: 17h03m - 17h41m Decl1950: -28.8° to -33.4°. II. Open star cluster TR 28. Catalogue of 76 stars and identification map Authors: Antalová, A. Bibcode: 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. Bibcode: 1971BAICz..22..352A Altcode: No abstract at ADS Title: UBV photographic photometry of stars in the region AR1950 17h03m - 17h41m Decl1950:-28.8° - 33.4°. I. The catalogue and identification maps of 250 OB and 101 photometrically interesting stars Authors: Antalová, A. Bibcode: 1970BAICz..21..331A Altcode: No abstract at ADS Title: Shape and evolution of photospheric regions with radiobursts IV flares Authors: Antalová, A. Bibcode: 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. Bibcode: 1967BAICz..18...61A Altcode: No abstract at ADS Title: Principal Characteristics of the 11-Year Solar Activity Cycle Authors: Antalova, A.; Gnevyshev, M. N. Bibcode: 1965SvA.....9..198A Altcode: No abstract at ADS Title: Interdependence of sunspot proper-motions and chromospheric flares Authors: Antalová, A. Bibcode: 1965BAICz..16...32A Altcode: No abstract at ADS Title: Principal Characteristics of the 11-Year Solar Activity Cycle Authors: Antalova, A.; Gnevyshev, M. N. Bibcode: 1965AZh....42..253A Altcode: No abstract at ADS Title: Proper motions of H- and J-type sunspots Authors: Antalová, A. Bibcode: 1963BAICz..14...97A Altcode: No abstract at ADS Title: Observations of Pluto in 1960 Authors: Antalová, A.; Antal, M. Bibcode: 1962BAICz..13...26A Altcode: No abstract at ADS Title: Photometric parameters of Comet Burnham 1959k Authors: Antalová, A.; Antal, M. Bibcode: 1961BAICz..12...71A Altcode: No abstract at ADS Title: Notes on the proper motions of late-type sunspots Authors: Antalová, A. Bibcode: 1961BAICz..12..108A Altcode: No abstract at ADS Title: The observations of Pluto in 1959 Authors: Antalová, A.; Antal, M. Bibcode: 1960BAICz..11..231A Altcode: No abstract at ADS