SAO-BNO Conference 2018

Международная конференция

Астрономия быстрого реагирования: гамма-всплески,
электромагнитное отождествление нейтринных событий и источников гравитационных волн

7-14 октября 2018 г.     Нижний Архыз (САО) и Терскол (БНО)

English / Русский

Орг.взнос и проживание



SAO main page
Специальная астрофизическая обсерватория РАН

BNO page
Баксанская нейтринная обсерватория ИЯИ РАН


(Программа предварительная. Возможны изменения и уточнения.)

7 октября, воскресенье. День приезда.

Будет организовано несколько рейсов транспорта из аэропорта Минеральные Воды в Нижний Архыз по мере прибытия участников Конференции.
15:00 - 18:00   Регистрация
18:00 - 20.00    Welcome party

8 октября, понедельник.

9:00 - 9:10    The Conference opening (V.V. Vlasyuk, V.B. Petkov, V.V. Sokolov)
     Section: Multimessenger, neutrino, gamma and gravitation astronomy
9:10 - 9:40   V.B. Petkov (BNO INR RAS). The multi-messenger astronomy: experiments in the Baksan Neutrino Observatory.
09:40 - 10:10   Vlasyuk V.V. International collaboration and facilities of SAO RAS in alert observations.
10:10 - 10:40   Lorenzo Amati The Transient High-Energy Sky and Early Universe Surveyor (THESEUS)
    The Transient High-Energy Sky and Early Universe Surveyor (THESEUS) is a mission concept developed in the last years by a large European consortium. As detailed in Amati et al. 2017 (arXiv:1710.04638) and Stratta et al. 2017 (arXiv:1712.08153), THESEUS aims at exploiting high-redshift GRBs for getting unique clues to the early Universe and, being an unprecedentedly powerful machine for the detection, accurate location (from ~arcmin to ~arcsec) and redshift determination of all types of GRBs (long, short, ~high-z, under-luminous, ultra-long) and many other classes of transient sources and phenomena, at providing a substantial contribution to multi-messenger time-domain astrophysics. Under these respects, THESEUS will show a beautiful synergy with the large observing facilities of the future, like E-ELT, TMT, SKA, CTA, ATHENA, in the electromagnetic domain, as well as with next-generation gravitational-waves and neutrino detectors, thus enhancing importantly their scientific return.
10:40 - 11:10               Перерыв на чай, кофе
11:10 - 11:40   Shashi Bhushan Pandey The 3.6m DOT and study of energetic cosmic transients
11:40 - 12:10   Fabrika S.N. First observations with new robotic telescopes of SAO RAS.
12:10 - 14:00               Перерыв на обед.
14:00 - 14:30   A.J.Castro-Tirado The monitoring of gamma-ray burst afterglows and search for optical counterparts to neutrino events and gravitational wave signals
14:30 - 15:00   Sokolov V.V. The search, identification and follow-up of new GRB optical afterglows by using the fast photometrical variability, the imaging in the BVRI bands and spectroscopy with BTA
15:00 - 15:30   Agnieszka Janiuk Astrophysical sources of gravitational radiation
    In this talk, I will discuss the possible origin, cosmic environment, and fate of the binary compact objects responsible for gravitational wave radiation detected so far. First, I will present the LIGO assembly of binary black holes that was established since the discovery of GW150914. These systems contain very massive black holes, whose origin poses a puzzle for the stellar evolution models. One of the possibilities is a process of direct collapse of massive stars. The feedback from a rotationally supported innermost parts of the star during the collapse may however help unbind the outer layers and halt accretion.
    This will have a consequence for both the ultimate mass of the black hole, and its resultant spin. I will also discuss the possible electromagnetic counterparts of the gravitational wave sources. The binary neutron star merger GW170817 was connected with the gamma ray emission observed as a weak short burst, which peculiar properties pose constraints for its progenitor model. Moreover, at lower energies the follow-up surveys have shown the presence of a kilonova emission from the merger's dynamical ejecta. These ejecta masses are broadly consistent with the estimated r-process production rate, required before to explain the Milky Way isotopes abundances. It is possible that the magnetically driven winds launched due to the accretion in the GRB central ngine may also contribute to the kilonova emission from NS-NS merger. Finally, the electromagnetic signal is in general not expected from a BH-BH merger. However, the wear transient detected by Fermi GBM detector 0.4 seconds after GW 150914 has been generating much speculation. I will briefly present the scenarios that aimed to account for such a coincident signal.
15:30 - 16 :00              Перерыв на чай, кофе
16:00 - 16:30   Beskin G.M. Search and study of optical transients with MiniMegaTORTORA.
16:30 - 17:00   Trushkin S. A., Fabrika S., Tsybulev P., Nizhelskij N.A., Bursov N. N. Search of fast radio bursts. The first year of the blind survey at 4.7 GHz with RATAN radio telescope

9 октября, вторник.

09:00 - 09:30   Gress O.A. The search and study of optical follow-up of gamma-ray bursts and sources of gravitational waves with the robotic telescope MASTER-Tunka
09:30 - 10:00   Sergeev A.V. New results in detection of ultra-high-frequency variability
10:00 - 10:30   Volnova A. GRB 171205A / SN 2017 iuk: observations and modelling of the multi-colour light curve of the second-closest GRB-related supernova
    We present the multi-colour light curve of the SN 2017iuk associated to the GRB 171205A. It is the second-closest GRB-SN event after "classic" SN 1998bw. The light curve consists of several hundreds of data-points in BRIgri filters, obtained by more than 20 telescopes of IKI-GRB-Follow-up Network from the observatories all around the world.
    We present the numerical modelling of the light curve using the one-dimensional radiation hydrodynamical code STELLA and give estimates for the SN explosion energy and other parameters.
10:30 - 11 :00              Перерыв на чай, кофе
11:00 - 11:30   Moskvitin A.S. Observations of the superluminous supernova SN 2009de
    Superluminous SNe with the absolute magnitude M < -21 make up only about 0.1% of all SNe. A large amount of energy can be explained by different mechanisms that can not be easily distinguished in observations data. We present photometry and spectroscopy of distant superluminous supernova SN 2009de located at z = 0.31, as well as modeling of the physical properties of it's host galaxy observed with the 6-m BTA in BVRI bands.
11:30 - 12:00    Xin Liping The observations of GRB afterglows and the plan to search for optical counterparts of gravitational wave.
12:00 - 12:30   Ikhsanov N. Preliminary title
12:30 - 14:00               Перерыв на обед.
14:00 - 14:30   Liang Enwei Magnetar as Central Engine of Gamma-Ray Bursts: Central Engine-Jet Connection, Wind-Jet Energy Partition, and Origin of Some Ultra-Long Bursts
14:30 - 15:00   Zhang Jin Radiation Properties of the Jets in AGNs: from the Core to Extended Regions
15:00 - 15:30    Wang Xiang-Gao Gamma-ray Burst Afterglow and GRBs Observing Plan
15:30 - 15:35    Lu Ruijing Preliminary title (Poster)
15:35 - 15:40   Balakina E.A. Supernova detection at the next-generation surveys (Poster)
15:40 - 15:45   Avakyan A.L., Malanchev K., Lipunova G. Accretion disk wind influence on the evolution of LMXB outburst (Poster)
According to the light curves obtained from observations of LMXB (Low-Mass X-ray Binary), within the framework of the Shakura-Sunyaev model it was found that the alpha viscosity parameter, which characterizes the mass transport in the accretion disk, lies in the range of 0.2-1. But simulations of the magnetorotational instability give values an order of magnitude smaller (about 0.03). In this work, we considered an additional source of matter transfer, namely, wind. We simulated the disk with the influence of the wind, which can decrease value of alpha parameter. As the result we receive the dependence of the change in the alpha on wind parameters. And if the decrease in alpha parameter is strong enough we conclude that the presence of wind can strongly affect the viscosity value, as well as the entire evolution of the disk as a whole.
15:45 - 15:50   Tavleev A.S., Malanchev K., Lipunova G. Vertical structure of accretion disks in LMXB (Poster)
LMXB (Low-mass X-ray binary) is a binary system where one of the components is either a neutron star or a black hole. The other component (donor, usually main sequence star) fills its Roche lobe and therefore accretes mass to the compact object. This leads to the formation of the accretion disk. The vertical structure of the accretion disk is calculated. We use a flexible calculation system, a choice of the equation of state, the opacity law and the chemical composition depends on the model. Our calculations can improve the accuracy of the modeling of LMXB outbursts.
15:50 - 16 :20              Coffee break
16:20 - 17 :30              Discussion

10 октября, среда

     Section: Low-background experiment
09:00 - 09:30   Kochkarov M.M. Fast neutrons in the Baksan Underground Scintillation Telescope: a background for core-collapse supernova searches.
09:30 - 10:00   A.S. LidvanskyTwo ultra-high energy gamma-ray bursts registered by the Carpet complex of BNO
10:00 - 10:30   Kuzminov V.V. Results of three years search for the 213Po half-life variations
10:30 - 11:00               Перерыв на чай, кофе
11:00 - 11:30   Gangapshev A.M. Recent results of search for hadronic axions at BNO
11:30 - 12:00    Sinev V.V. Solar CNO neutrinos or terrestrial 40K antineutrinos?
    The Earth thermal flux value varies from 50 up to 250 TW according different estimations. Upper limit could be achieved only if potassium abundance in the Earth exceeds 2%. In Borexino data the valley between beryllium neutrinos and 11C spectrum is filled with betas from 210Bi. But it also contains CNO neutrinos. CNO cycle in the Sun could be depressed according to last researches. This means that part of CNO spectrum could be from terrestrial 40K antineutrinos because their spectra are very similar.
12:00 - 14:00               Перерыв на обед.
14:00 - 14:30   Kazalov V.V. Search for double K-capture of Xe-124 with the large volume copper proportional counter.
14:30 - 15:00   R.V. Novoseltseva, M.M. Boliev, I.M. Dzaparova, M.M Kochkarov, A.N. Kurenya, Yu. F. Novoseltsev, V.B. Petkov, P.S.Striganov, A.F. Yanin A search for neutrino bursts in the Galaxy at the Baksan Underground Scintillation Telescope; 38 years of exposure
    The Baksan Underground Scintillation Telescope has been operating under the program of searching for neutrino bursts since the middle of 1980. The target is two parts of the facility, the D1 and the D2, with the total scintillator mass of 240 t. The count rates of background events are 0.02 s -1 in the D1 and 0.12 s -1 in the D2. The actual observation time over the period from June 30, 1980, to December 31, 2017, is 32.1 years. No candidate for the stellar core collapse has been detected during the observation period. The upper bound for the mean rate of the supernova core collapse in our Galaxy is 0.072y -1 (90% CL).
15:00 - 15:30   D.D. Dzhappuev Limits on the isotropic diffuse gamma-ray flux between 100 TeV and 1 PeV: experiments Carpet-2 and Carpet-3
15:30 - 16:00               Перерыв на чай, кофе
16:00 - 18:30          Excursion to the 6-meter telescope BTA

11 октября, четверг.

9:00 - 9:30   A.F. Yanin Scintillation detectors based on the SiPM matrices: prospects for the large volume neutrino detectors
09:30 - 10:00   A.N. Kurenya DAQ system for the complex of the BUST – Andyrchy – Carpet-2 facilities
10:00 - 10:30   Semenov S.V.Neutrino interaction with nuclei
10:30 - 11:00               Перерыв на чай, кофе
11:00 - 11:30   M.M. Boliev Search for astrophysical neutrino sources at the Baksan Underground Scintillation Telescope
11:30 - 12:00   Shibanov Yu.A. Direct observations of transformation of low-massive binaries to millisecond radio pulsars and back
12:30 - 14:00               Перерыв на обед.
     Section: Compact astrophysical objects and the QCD phase transition
14:00 - 14:30    Gong Yungui On the polarization of gravitational waves in alternative theories of gravity
    According to the Newman-Penrose formalism, in general there are six polarizations for general theories of gravity. In particular, the presence of the longitudinal mode means that the theory has all six polarizations. For massive scalar-tensor theory of gravity or f(R) theory, the longitudinal mode presents, but the theory has only three dynamical degrees of freedom, it seems that there is inconsistency somewhere. We point out that the Newman-Penrose formalism is not directly applicable to massive mode, the polarization of the massive scalar field is a mix of breathing and longitudinal mode and the longitudinal mode is proportional to the mass, when the mass becomes zero, the mix mode becomes the pure breathing mode which is consistent with the Newman-Penrose formalism. Since the longitudinal mode is proportional to the mass, so it can be detected only in very low frequency band, like the PTA band. The result is fundamentally important for the understanding of the nature of gravity. If we only detect the plus and cross polarizations, then we know that graviton is massless spin 2 particle. In addition to the plus and cross polarizations, if we also detect the breathing polarization, then we know that gravitation is mediated by both massless spin 2 and spin 0 particles. Apart from the above three polarizations, if we also detect the longitudinal polarization, then we know that gravitation propagated by massless spin 2 and massive spin 0 particles.
14:30 - 15:00   Grzegorz Wiktorowicz New results in studying strange quark stars
15:00 - 15:30   Oschepkov S.A., Raikov A.A., Baryshev Yu.V. Mass-radius relation for relativistic compact objects in geometrical and field gravitation theories.
15:30 - 16:00   Fabrika S.N., Sholukhova O.N., Vinokurov A.S.Recent achievements in studying ULXs and other related objects.
16:30 - 17:00               Перерыв на чай, кофе
17:00 - 19:00          Excursion to the radio telescope RATAN-6000

12 октября, пятница.

     Section: GRBs and cosmology
9:00 - 9:30   Atilla Meszaros The spatial distribution of GRBs (both in redshift and in the angular sky position)
09:30 - 10:00   Raikov A.A., Sokolov V.V., Baryshev Yu.V., Shirokov S.I. Gamma-ray bursts as an instrument for testing cosmological models
10:00 - 10:30   Baryshev Yu.V., Oschepkov S.A. Gravitational mechanism for origin and collimation of jets from relativistic compact objects
10:30 - 11:00   Sokolov V.V., Baryshev Yu.V., et al. Gamma-Ray Bursts and testing the nature of cosmological redshift
History of the problem. GRB as a tool for cosmology. Universality for all frequences. GRB puls structure. Afterglow and SN light-curves. Perspectives for observations ..
11:00 - 11:30              Перерыв на чай, кофе
11:30 - 12:00   Atilla Meszaros The diversity of GRBs statistically (is there a third group? physical meaning? relation to XRFs?)
12:00 - 12:30   Makarov D.I. Structure of the Local Universe
12:00 - 12:30   I.V.Sokolov, I.A. Solovyev The field galaxies clustering in GRBs lines of sights based on the BTA observations
12:30 - 13:00   A. N. Baushev, L. del Valle, L. E. Campusano, A. Escala, R. R. Muñoz, G. A. Palma Cusps in the center of galaxies: a real conflict with observations or a numerical artefact of cosmological simulations?
13:00 - 14:30               Перерыв на обед
14:30 - 17:00               General discussion
19:00   Farewell party

13 октября, суббота.

09:00 - 18:00             Excursion to Baksan Neutrino Observatory or to Arkhyz

14 октября, воскресенье.

   Leaving Nizhnij Arkhyz

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