Prompt, early, and afterglow optical observations of five gamma-ray bursts (GRBs 100901A, 100902A, 100905A, 100906A, and 101020A)

We present results of the prompt, early, and afterglow optical observations of five gamma-ray bursts, GRBs 100901A, 100902A, 100905A, 100906A, and 101020A, made with the Mobile Astronomical System of TElescope-Robots in Russia (MASTER-II net), the 1.5-m telescope of Sierra-Nevada Observatory, and the 2.56-m Nordic Optical Telescope. For two sources, GRB 100901A and GRB 100906A, we detected optical counterparts and obtained light curves starting before cessation of gamma-ray emission, at 113 s and 48 s after the trigger, respectively. Observations of GRB 100906A were conducted with two polarizing filters. Observations of the other three bursts gave the upper limits on the optical flux; their properties are briefly discussed. More detailed analysis of GRB 100901A and GRB 100906A supplemented by Swift data provides the following results and indicates different origins of the prompt optical radiation in the two bursts. The light curves patterns and spectral distributions suggest a common production site of the prompt optical and high-energy emission in GRB 100901A. Results of spectral fits for GRB 100901A in the range from the optical to X-rays favor power-law energy distributions with similar values of the optical extinction in the host galaxy. GRB 100906A produced a smoothly peaking optical light curve suggesting that the prompt optical radiation in this GRB originated in a front shock. This is supported by a spectral analysis. We have found that the Amati and Ghirlanda relations are satisfied for GRB 100906A. An upper limit on the value of the optical extinction on the host of GRB 100906A is obtained.Comment: 18 pages, 14 figures, 14 tables, 5 machine readable tables; accepted for publication in MNRA

The MASTER-II network of robotic optical telescopes. First results

The main stages in the creation of the Russian segment of the MASTER network of robotic telescopes is described. This network is designed for studies of the prompt optical emission of gammaray bursts (GRBs; optical emission synchronous with the gamma-ray radiation) and surveys of the sky aimed at discovering uncataloged objects and photometric studies for various programs. The first results obtained by the network, during its construction and immediately after its completion in December 2010, are presented. Eighty-nine alert pointings at GRBs (in most cases, being the first ground telescopes to point at the GRBs) were made from September 2006 through July 2011. The MASTER network holds first place in the world in terms of the total number of first pointings, and currently more than half of first pointings at GRBs by ground telescopes are made by the MASTER network. Photometric light curves of GRB 091020, GRB 091127, GRB 100901A, GRB 100906A, GRB 10925A, GRB 110106A, GRB 110422A, and GRB 110530A are presented. It is especially important that prompt emission was observed for GRB 100901A and GRB 100906A, and thar GRB 091127, GRB 110422A, and GRB 110106A were observed from the first seconds in two polarizations. Very-wide-field cameras carried out synchronous observations of the prompt emission of GRB 081102, GRB 081130B, GRB 090305B, GRB 090320B, GRB 090328, and GRB 090424. Discoveries of Type Ia supernovae are ongoing (among them the brightest supernova in 2009): 2008gy, 2009nr, 2010V, and others. In all, photometry of 387 supernovae has been carried out, 43 of which were either discovered or first observed with MASTER telescopes; more than half of these are Type Ia supernovae. Photometric studies of the open clusters NGC 7129 and NGC 7142 have been conducted, leading to the discovery of 38 variable stars. Sixty-nine optical transients have been discovered. © 2013 Pleiades Publishing, Ltd

A Reverse Shock in GRB 181201A

We present comprehensive multiwavelength radio to X-ray observations of GRB 181201A spanning from ≈150 s to ≈163 days after the burst, comprising the first joint ALMA-VLA-GMRT observations of a gamma-ray burst (GRB) afterglow. The radio and millimeter-band data reveal a distinct signature at ≈3.9 days, which we interpret as reverse-shock (RS) emission. Our observations present the first time that a single radio-frequency spectral energy distribution can be decomposed directly into RS and forward shock (FS) components. We perform detailed modeling of the full multiwavelength data set, using Markov Chain Monte Carlo sampling to construct the joint posterior density function of the underlying physical parameters describing the RS and FS synchrotron emission. We uncover and account for all discovered degeneracies in the model parameters. The joint RS-FS modeling reveals a weakly magnetized (σ ≈ 3 × 10-3), mildly relativistic RS, from which we derive an initial bulk Lorentz factor of Γ0 ≈ 103 for the GRB jet. Our results support the hypothesis that low-density environments are conducive to the observability of RS emission. We compare our observations to other events with strong RS detections and find a likely observational bias selecting for longer lasting, nonrelativistic RSs. We present and begin to address new challenges in modeling posed by the present generation of comprehensive, multifrequency data sets

Multi-messenger observations of a binary neutron star merger

On 2017 August 17 a binary neutron star coalescence candidate (later designated GW170817) with merger time 12:41:04 UTC was observed through gravitational waves by the Advanced LIGO and Advanced Virgo detectors. The Fermi Gamma-ray Burst Monitor independently detected a gamma-ray burst (GRB 170817A) with a time delay of ~1.7 s with respect to the merger time. From the gravitational-wave signal, the source was initially localized to a sky region of 31 deg2 at a luminosity distance of 40+8-8 Mpc and with component masses consistent with neutron stars. The component masses were later measured to be in the range 0.86 to 2.26 Mo. An extensive observing campaign was launched across the electromagnetic spectrum leading to the discovery of a bright optical transient (SSS17a, now with the IAU identification of AT 2017gfo) in NGC 4993 (at ~40 Mpc) less than 11 hours after the merger by the One- Meter, Two Hemisphere (1M2H) team using the 1 m Swope Telescope. The optical transient was independently detected by multiple teams within an hour. Subsequent observations targeted the object and its environment. Early ultraviolet observations revealed a blue transient that faded within 48 hours. Optical and infrared observations showed a redward evolution over ~10 days. Following early non-detections, X-ray and radio emission were discovered at the transient’s position ~9 and ~16 days, respectively, after the merger. Both the X-ray and radio emission likely arise from a physical process that is distinct from the one that generates the UV/optical/near-infrared emission. No ultra-high-energy gamma-rays and no neutrino candidates consistent with the source were found in follow-up searches. These observations support the hypothesis that GW170817 was produced by the merger of two neutron stars in NGC4993 followed by a short gamma-ray burst (GRB 170817A) and a kilonova/macronova powered by the radioactive decay of r-process nuclei synthesized in the ejecta

Ранние оптические наблюдения семи гамма-всплесков в сравнении с их гамма-рентгеновскими характеристиками на глобальной сети телескопов-роботов МГУ МАСТЕР

Seven gamma-ray bursts – GRB 130907A, GRB 140311B, GRB 140129B, GRB 160227A, GRB 120404A, GRB 110801A, and GRB 120811C were observed by the MSU MASTER (Mobile Astronomical System of TElescope Robots) Global Network. Full automation of the observations provided for obtaining unique data on the properties of early optical radiation accompanying gamma-ray bursts. The data are compared in the optical (MASTER), X-ray (SWIFT X-ray Telescope, XRT) and gamma (SWIFT Burst Alert Telescope, BAT) ranges. Based on the data obtained, two groups are identified, and their radiation mechanisms are revealed. The effect of gamma-ray bursts on the biosphere of the Earth is determined, and the estimates and the scale of such an effect are considered.В статье представлены результаты наблюдений семи гамма-всплесков – GRB 130907A, GRB 140311B, GRB 140129B, GRB 160227A, GRB 120404A, GRB 110801A, GRB 120811C, полученные на телескопах-роботах глобальной сети МГУ «МАСТЕР». Полная автоматизация наблюдений позволила получить уникальные данные о свойствах раннего оптического излучения, сопровождавшего гамма-всплески. Выполнено сравнение данных в оптическом (МАСТЕР), рентгеновском (SWIFTX-rayTelescope (XRT)) и гамма (SWIFTBurstAlertTelescope (BAT)) диапазонах. На основании полученных данных выделены две группы, для которых определен механизм излучения. Также определено воздействие гамма-всплесков на биосферу Земли и рассмотрены оценки и масштаб такого влияния

Multi-messenger Observations of a Binary Neutron Star Merger

On 2017 August 17 a binary neutron star coalescence candidate (later designated GW170817) with merger time 12:41:04 UTC was observed through gravitational waves by the Advanced LIGO and Advanced Virgo detectors. The Fermi Gamma-ray Burst Monitor independently detected a gamma-ray burst (GRB 170817A) with a time delay of ∼ 1.7 {{s}} with respect to the merger time. From the gravitational-wave signal, the source was initially localized to a sky region of 31 deg2 at a luminosity distance of {40}-8+8 Mpc and with component masses consistent with neutron stars. The component masses were later measured to be in the range 0.86 to 2.26 {M}ȯ . An extensive observing campaign was launched across the electromagnetic spectrum leading to the discovery of a bright optical transient (SSS17a, now with the IAU identification of AT 2017gfo) in NGC 4993 (at ∼ 40 {{Mpc}}) less than 11 hours after the merger by the One-Meter, Two Hemisphere (1M2H) team using the 1 m Swope Telescope. The optical transient was independently detected by multiple teams within an hour. Subsequent observations targeted the object and its environment. Early ultraviolet observations revealed a blue transient that faded within 48 hours. Optical and infrared observations showed a redward evolution over ∼10 days. Following early non-detections, X-ray and radio emission were discovered at the transient’s position ∼ 9 and ∼ 16 days, respectively, after the merger. Both the X-ray and radio emission likely arise from a physical process that is distinct from the one that generates the UV/optical/near-infrared emission. No ultra-high-energy gamma-rays and no neutrino candidates consistent with the source were found in follow-up searches. These observations support the hypothesis that GW170817 was produced by the merger of two neutron stars in NGC 4993 followed by a short gamma-ray burst (GRB 170817A) and a kilonova/macronova powered by the radioactive decay of r-process nuclei synthesized in the ejecta.</p

Early Optical Observations of Gamma-Ray Bursts Compared with Their Gamma- and X-Ray Characteristics Using a MASTER Global Network of Robotic Telescopes from Lomonosov Moscow State University

We present the results of early observations for 130 error-boxes of gamma-ray bursts performed with the Mobile Astronomical System of TElescope-Robots (MASTER) global network of robotic telescopes from Moscow State University in fully automatic mode (2011?2017). Among them, GRB 130907A, GRB 120811C, GRB 110801A, GRB 120404A, GRB 140129B, GRB140311B, and GRB 160227A are considered in details. Among these 130 gamma-ray bursts, in the first 60 s after the trigger with the Swift, Fermi, INTEGRAL, MAXI, Lomonosov, and Konus-Wind orbital observatories, the MASTER was pointed on 51 gamma-ray bursts, being the leader in terms of the first pointing. Full observation automation and MASTER own real-time image processing software allowed us to obtain unique data on early optical emission that accompanied 44 gamma-ray bursts (GRB 110801A, GRB120106A, GRB 120404A, GRB 120811C, GRB 120907A, GRB 121011A, GRB 130122A, GRB 130907A, GRB 131030A, GRB 131125A, GRB 140103A, GRB 140108A, GRB 140129B, GRB 140206A, GRB 140304A, GRB 140311B, GRB 140512A, GRB 140629A, GRB 140801A, GRB140907A, GRB 140930B, GRB141028A, GRB 141225A, GRB 150210A, GRB 150211A, GRB 150301B, GRB 150323C, GRB 150404A/Fermi trigger 449861706, GRB 150403A, GRB 150413A, GRB 150518A, GRB 150627A, GRB 151021A, GRB 151215A, GRB 160104A, GRB 160117B, GRB 160131A, GRB 160227A, GRB 160425A, GRB 160611A, GRB 160625B, GRB 160804A, GRB 160910A, GRB 161017A, GRB 161117A, GRB 161119A). We obtain light curves for 13 gamma-ray bursts among the above listed ones and compare the data in the optical (MASTER), X-ray (Swift-XRT), and hard X-ray (Swift-BAT) ranges.We present the results of early observations for 130 error-boxes of gamma-ray bursts performed with the Mobile Astronomical System of TElescope-Robots (MASTER) global network of robotic telescopes from Moscow State University in fully automatic mode (2011?2017). Among them, GRB 130907A, GRB 120811C, GRB 110801A, GRB 120404A, GRB 140129B, GRB140311B, and GRB 160227A are considered in details. Among these 130 gamma-ray bursts, in the first 60 s after the trigger with the Swift, Fermi, INTEGRAL, MAXI, Lomonosov, and Konus-Wind orbital observatories, the MASTER was pointed on 51 gamma-ray bursts, being the leader in terms of the first pointing. Full observation automation and MASTER own real-time image processing software allowed us to obtain unique data on early optical emission that accompanied 44 gamma-ray bursts (GRB 110801A, GRB120106A, GRB 120404A, GRB 120811C, GRB 120907A, GRB 121011A, GRB 130122A, GRB 130907A, GRB 131030A, GRB 131125A, GRB 140103A, GRB 140108A, GRB 140129B, GRB 140206A, GRB 140304A, GRB 140311B, GRB 140512A, GRB 140629A, GRB 140801A, GRB140907A, GRB 140930B, GRB141028A, GRB 141225A, GRB 150210A, GRB 150211A, GRB 150301B, GRB 150323C, GRB 150404A/Fermi trigger 449861706, GRB 150403A, GRB 150413A, GRB 150518A, GRB 150627A, GRB 151021A, GRB 151215A, GRB 160104A, GRB 160117B, GRB 160131A, GRB 160227A, GRB 160425A, GRB 160611A, GRB 160625B, GRB 160804A, GRB 160910A, GRB 161017A, GRB 161117A, GRB 161119A). We obtain light curves for 13 gamma-ray bursts among the above listed ones and compare the data in the optical (MASTER), X-ray (Swift-XRT), and hard X-ray (Swift-BAT) ranges.Fil: Ershova, O. A.. Irkutsk State University; RusiaFil: Ershova, O. A.. Irkutsk State University; RusiaFil: Lipunov, Vladimir. Lomonosov Moscow State University. Sternberg Astronomical Institute; RusiaFil: Lipunov, Vladimir. Lomonosov Moscow State University. Sternberg Astronomical Institute; RusiaFil: Gorbovskoy, E. S.. Lomonosov Moscow State University. Sternberg Astronomical Institute; RusiaFil: Gorbovskoy, E. S.. Lomonosov Moscow State University. Sternberg Astronomical Institute; RusiaFil: Tyurina, N. V.. Lomonosov Moscow State University. Sternberg Astronomical Institute; RusiaFil: Tyurina, N. V.. Lomonosov Moscow State University. Sternberg Astronomical Institute; RusiaFil: Kornilov, V. G.. Lomonosov Moscow State University. Sternberg Astronomical Institute; RusiaFil: Kornilov, V. G.. Lomonosov Moscow State University. Sternberg Astronomical Institute; RusiaFil: Zimnukhov, D. S.. Lomonosov Moscow State University. Sternberg Astronomical Institute; RusiaFil: Zimnukhov, D. S.. Lomonosov Moscow State University. Sternberg Astronomical Institute; RusiaFil: Gabovich, A. Lomonosov Moscow State University. Sternberg Astronomical Institute; RusiaFil: Gabovich, A. Lomonosov Moscow State University. Sternberg Astronomical Institute; RusiaFil: Gress, O. A.. Lomonosov Moscow State University. Sternberg Astronomical Institute; RusiaFil: Gress, O. A.. Lomonosov Moscow State University. Sternberg Astronomical Institute; RusiaFil: Budnev, N. M.. rkutsk State University; RusiaFil: Budnev, N. M.. rkutsk State University; RusiaFil: Yurkov, V. V.. Blagoveshchensk State Pedagogical University; RusiaFil: Yurkov, V. V.. Blagoveshchensk State Pedagogical University; RusiaFil: Vladimirov, V. V.. Lomonosov Moscow State University. Sternberg Astronomical Institute; RusiaFil: Vladimirov, V. V.. Lomonosov Moscow State University. Sternberg Astronomical Institute; RusiaFil: Kuznetsov. A. S.. Lomonosov Moscow State University. Sternberg Astronomical Institute; RusiaFil: Kuznetsov. A. S.. Lomonosov Moscow State University. Sternberg Astronomical Institute; RusiaFil: Balanutsa, P. V.. Lomonosov Moscow State University. Sternberg Astronomical Institute; RusiaFil: Balanutsa, P. V.. Lomonosov Moscow State University. Sternberg Astronomical Institute; RusiaFil: Rebolo, R.. Instituto de Astrofisica de Canarias; EspañaFil: Rebolo, R.. Instituto de Astrofisica de Canarias; EspañaFil: Serra Ricart, M.. Instituto de Astrofisica de Canarias; EspañaFil: Serra Ricart, M.. Instituto de Astrofisica de Canarias; EspañaFil: Buckley, D.. South African Astrophysical Observatory; SudáfricaFil: Buckley, D.. South African Astrophysical Observatory; SudáfricaFil: Podestá, Ricardo César. Universidad Nacional de San Juan; ArgentinaFil: Podestá, Ricardo César. Universidad Nacional de San Juan; ArgentinaFil: Levato, Orlando Hugo. Consejo Nacional de Investigaciones Científicas y Técnicas. Centro Científico Tecnológico Conicet - San Juan. Instituto de Ciencias Astronómicas, de la Tierra y del Espacio. Universidad Nacional de San Juan. Instituto de Ciencias Astronómicas, de la Tierra y del Espacio; ArgentinaFil: Levato, Orlando Hugo. Consejo Nacional de Investigaciones Científicas y Técnicas. Centro Científico Tecnológico Conicet - San Juan. Instituto de Ciencias Astronómicas, de la Tierra y del Espacio. Universidad Nacional de San Juan. Instituto de Ciencias Astronómicas, de la Tierra y del Espacio; ArgentinaFil: Lopez, Carlos. Universidad Nacional de San Juan; ArgentinaFil: Lopez, Carlos. Universidad Nacional de San Juan; ArgentinaFil: Podesta, Federico. Universidad Nacional de San Juan; ArgentinaFil: Podesta, Federico. Universidad Nacional de San Juan; ArgentinaFil: Francile, Carlos Natale. Universidad Nacional de San Juan; ArgentinaFil: Francile, Carlos Natale. Universidad Nacional de San Juan; ArgentinaFil: Mallamaci, Claudio Carlos. Universidad Nacional de San Juan; ArgentinaFil: Mallamaci, Claudio Carlos. Universidad Nacional de San Juan; ArgentinaFil: Yazev, S. A.. Irkutsk State University; RusiaFil: Yazev, S. A.. Irkutsk State University; RusiaFil: Vlasenko, D. M.. Lomonosov Moscow State University. Sternberg Astronomical Institute; RusiaFil: Vlasenko, D. M.. Lomonosov Moscow State University. Sternberg Astronomical Institute; RusiaFil: Tlatov, A.. Russian Academy of Sciences; RusiaFil: Tlatov, A.. Russian Academy of Sciences; RusiaFil: Senik, V.. Irkutsk State University; RusiaFil: Senik, V.. Irkutsk State University; RusiaFil: Grinshpun, V.. Moscow State University. Physics Department; RusiaFil: Grinshpun, V.. Moscow State University. Physics Department; RusiaFil: Chasovnikov, A.. Lomonosov Moscow State University. Physics Department; RusiaFil: Chasovnikov, A.. Lomonosov Moscow State University. Physics Department; RusiaFil: Topolev, V.. Moscow State University. Physics Department; RusiaFil: Topolev, V.. Moscow State University. Physics Department; RusiaFil: Pozdnyakov, A.. Moscow State University. Physics Department; RusiaFil: Pozdnyakov, A.. Moscow State University. Physics Department; RusiaFil: Zhirkov, K.. Moscow State University. Physics Department; RusiaFil: Zhirkov, K.. Moscow State University. Physics Department; RusiaFil: Kuvshinov, D.. Lomonosov Moscow State University. Sternberg Astronomical Institute; RusiaFil: Kuvshinov, D.. Lomonosov Moscow State University. Sternberg Astronomical Institute; RusiaFil: Balakin, F.. Moscow State University. Physics Department; RusiaFil: Balakin, F.. Moscow State University. Physics Department; Rusi

Early optical observations of seven gamma-ray bursts in comparison to their gamma X-ray characteristics in the MSU MASTER Global Robotic Telescopes Net

Seven gamma-ray bursts – GRB 130907A, GRB 140311B, GRB 140129B, GRB 160227A, GRB 120404A, GRB 110801A, and GRB 120811C were observed by the MSU MASTER (Mobile Astronomical System of TElescope Robots) Global Network. Full automation of the observations provided for obtaining unique data on the properties of early optical radiation accompanying gamma-ray bursts. The data are compared in the optical (MASTER), X-ray (SWIFT X-ray Telescope, XRT) and gamma (SWIFT Burst Alert Telescope, BAT) ranges. Based on the data obtained, two groups are identified, and their radiation mechanisms are revealed. The effect of gamma-ray bursts on the biosphere of the Earth is determined, and the estimates and the scale of such an effect are considered

MASTER Optical Detection of the First LIGO/Virgo Neutron Star Binary Merger GW170817

Following the discovery of the gravitational-wave source GW170817 by three Laser Interferometer Gravitational-wave Observatory (LIGO)/Virgo antennae (Abbott et al., 2017a), the MASTER Global Robotic Net telescopes obtained the first image of the NGC 4993 host galaxy. An optical transient, MASTER OTJ130948.10-232253.3/SSS17a was later found, which appears to be a kilonova resulting from the merger of two neutron stars (NSs). Here we describe this independent detection and photometry of the kilonova made in white light, and in B, V, and R filters. We note that the luminosity of this kilonova in NGC 4993 is very close to those measured for other kilonovae possibly associated with gamma-ray burst (GRB) 130603 and GRB 080503.Fil: Lipunov, V. M.. Lomonosov Moscow State University; RusiaFil: Gorbovskoy, E.. Lomonosov Moscow State University; RusiaFil: Kornilov, V. G.. Lomonosov Moscow State University; RusiaFil: Tyurina, N.. Lomonosov Moscow State University; RusiaFil: Balanutsa, P.. Lomonosov Moscow State University; RusiaFil: Kuznetsov, A.. Lomonosov Moscow State University; RusiaFil: Vlasenko, D.. Lomonosov Moscow State University; RusiaFil: Kuvshinov, D.. Lomonosov Moscow State University; RusiaFil: Gorbunov, I.. Lomonosov Moscow State University; RusiaFil: Buckley, D. A. H.. South African Astrophysical Observatory; SudáfricaFil: Krylov, A. V.. Lomonosov Moscow State University; RusiaFil: Podesta, R.. Universidad Nacional de San Juan. Facultad de Ciencias Exactas Físicas y Naturales. Departamento de Informática. Observatorio Astronómico Félix Aguilar; ArgentinaFil: Lopez, C.. Universidad Nacional de San Juan. Facultad de Ciencias Exactas Físicas y Naturales. Departamento de Informática. Observatorio Astronómico Félix Aguilar; ArgentinaFil: Podesta, F.. Universidad Nacional de San Juan. Facultad de Ciencias Exactas Físicas y Naturales. Departamento de Informática. Observatorio Astronómico Félix Aguilar; ArgentinaFil: Levato, Orlando Hugo. Consejo Nacional de Investigaciones Científicas y Técnicas. Centro Científico Tecnológico Conicet - San Juan. Instituto de Ciencias Astronómicas, de la Tierra y del Espacio. Universidad Nacional de San Juan. Instituto de Ciencias Astronómicas, de la Tierra y del Espacio; ArgentinaFil: Saffe, Carlos. Consejo Nacional de Investigaciones Científicas y Técnicas. Centro Científico Tecnológico Conicet - San Juan. Instituto de Ciencias Astronómicas, de la Tierra y del Espacio. Universidad Nacional de San Juan. Instituto de Ciencias Astronómicas, de la Tierra y del Espacio; ArgentinaFil: Mallamachi, C.. Universidad Nacional de San Juan; ArgentinaFil: Potter, S.. South African Astrophysical Observatory; SudáfricaFil: Budnev, N. M.. Irkutsk State University; RusiaFil: Gress, O.. Lomonosov Moscow State University; Rusia. Irkutsk State University; RusiaFil: Ishmuhametova, Yu.. Irkutsk State University; RusiaFil: Vladimirov, V.. Lomonosov Moscow State University; RusiaFil: Zimnukhov, D.. Lomonosov Moscow State University; RusiaFil: Yurkov, V.. Blagoveschensk State Pedagogical University; RusiaFil: Sergienko, Yu.. Blagoveschensk State Pedagogical University; RusiaFil: Gabovich, A.. Blagoveschensk State Pedagogical University; RusiaFil: Rebolo, R.. Instituto de Astrofísica de Canarias; EspañaFil: Serra Ricart, M.. Instituto de Astrofísica de Canarias; EspañaFil: Israelyan, G.. Instituto de Astrofísica de Canarias; EspañaFil: Chazov, V.. Lomonosov Moscow State University; RusiaFil: Wang, Xiaofeng. Tsinghua University; ChinaFil: Tlatov, A.. Kislovodsk Solar Observing Station of Pulkovo Observatory; RusiaFil: Panchenko, M. I.. Lomonosov Moscow State University; Rusi