Персона: Бакланов, Петр Валерьевич
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Институт ядерной физики и технологий
Цель ИЯФиТ и стратегия развития - создание и развитие научно-образовательного центра мирового уровня в области ядерной физики и технологий, радиационного материаловедения, физики элементарных частиц, астрофизики и космофизики.
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Петр Валерьевич
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- ПубликацияТолько метаданныеA Model for the Fast Blue Optical Transient AT2018cow: Circumstellar Interaction of a Pulsational Pair-instability Supernova(2020) Leung, S. -C.; Blinnikov, S.; Nomoto, K.; Sorokina, E.; Baklanov, P.; Бакланов, Петр Валерьевич© 2020. The American Astronomical Society. All rights reserved.The fast blue optical transient (FBOT) ATLAS18qqn (AT2018cow) has a light curve as bright as that of superluminous supernovae (SLSNe) but rises and falls much faster. We model this light curve by circumstellar interaction of a pulsational pair-instability (PPI) supernova (SN) model based on our PPISN models studied in previous work. We focus on the 42 Me He star (core of a 80 Me star) which has circumstellar matter (CSM) of mass 0.50 Me. With the parameterized mass cut and the kinetic energy of explosion E, we perform hydrodynamical calculations of nucleosynthesis and optical light curves of PPISN models. The optical light curve of the first ∼20 days of AT2018cow is well reproduced by the shock heating of CSM for the 42 Me He star with E = 5 × 1051 erg. After day 20, the light curve is reproduced by the radioactive decay of 0.6 M*56 Co, which is a decay product of 56Ni in the explosion. We also examine how the light-curve shape depends on the various model parameters, such as CSM structure and composition. We also discuss (1) other possible energy sources and their constraints, (2) the origin of the observed high-energy radiation, and (3) how our result depends on the radiative transfer codes. Based on our successful model for AT2018cow and the model for SLSN with CSM mass as large as 20 M*, we propose the working hypothesis that PPISN produces SLSNe if the CSM is massive enough and FBOTs if CSM is less than ∼1 Me
- ПубликацияТолько метаданныеStrongly Lensed Supernova Refsdal: Refining Time Delays Based on the Supernova Explosion Models(2021) Baklanov, P.; Lyskova, N.; Blinnikov, S.; Nomoto, K.; Бакланов, Петр ВалерьевичWe explore the properties of supernova (SN) "Refsdal"-the first discovered gravitationally lensed SN with multiple images. A large magnification provided by the galactic-scale lens, augmented by the cluster lens, gave us a unique opportunity to perform a detailed modeling of a distant SN at z similar or equal to 1.5. We present results of radiation hydrodynamics modeling of SN Refsdal. According to our calculations, the SN Refsdal progenitor is likely to be a more massive and energetic version of SN 1987A, i.e., a blue supergiant star with the following parameters: the progenitor radius R-0 = (50 +/- 1)R-circle dot, the total mass M-tot = (25 +/- 2)M-circle dot, the radioactive Ni-56 mass M-56Ni = (0.26 +/- 0.05) M-circle dot, and the total energy release E-burst = (4.7 +/- 0.8) x 10(51) erg. Reconstruction of SN light curves allowed us to obtain time delays and magnifications for the images S2-S4 relative to S1 with higher accuracy than previous template-based estimates of Rodney et al. (2016). The measured time delays are Delta t(S2-S1) = 9.5(-2.7)(+2.6) days, Delta t(S3-S1) = 4.2(-2.3)(+2.3) days, Delta t(S4-S1) = 30-(-7.8)(8.2) days. The obtained magnification ratios are mu(S2/S1) = 1.14 +/- 0.02, mu(S3/S1) = 1.01 +/- 0.02, and mu(S4/S1) = 0.35 +/- 0.02. We estimate the Hubble constant H-0 = 68.6(-9.7+)(13.6) km s(-1) Mpc(-1) via rescaling the time delays predicted by different lens models to match the values obtained in this work. With more photometric data on the fifth image SX, we will be able to further refine the time delay and magnification estimates for SX and obtain competitive constraints on H-0.
- ПубликацияТолько метаданныеOn the Modeling of Type IIP Supernovae in the Gray-Opacity Approximation and Properties of Their Light Curves(2022) Urvachev, E. M.; Blinnikov, S. I.; Glazyrin, S. I.; Baklanov, P. V.; Бакланов, Петр Валерьевич
- ПубликацияТолько метаданныеSN 2019edo: A Type II-P Supernova with a Fast Brightness Rise and a Short Plateau Phase(2022) Tsvetkov, D. Y.; Belinsky, A. A.; Ikonnikova, N. P.; Burlak, M. A.; Volkov, I. M.; Pavlyuk, N. N.; Baklanov, P. V.; Blinnikov, S. I.; Ushakova, M. G.; Echeistov, V. A.; Бакланов, Петр Валерьевич
- ПубликацияТолько метаданныеType II-P Supernova SN 2018aoq in NGC 4151: Light Curves, Models, and Distance(2021) Tsvetkov, D. Y.; Pavlyuk, N. N.; Vozyakova, O. V.; Shatsky, N. I.; Baklanov, P. V.; Бакланов, Петр Валерьевич© 2021, Pleiades Publishing, Inc.Abstract: The results of UBVRIJHK photometry for the type II-P supernova SN 2018aoq in NGC 4151 obtained from April 4, 2018, to January 14, 2019, with several telescopes, including the 2.5-m telescope at the Caucasus Mountain Observatory of the Sternberg Astronomical Institute of the Moscow State University, are presented. The main parameters of its light curves have been determined. The light and color curves of SN 2018aoq and several well-studied SNe II-P are compared. SN 2018aoq is shown to be intermediate in peak luminosity between SNe II-P with normal and reduced luminosities. Radiation-hydrodynamics simulations of the light curves and velocities of the expanding envelope of SN 2018aoq have been performed using the STELLA code. The best agreement with the observations has been achieved for SN progenitor models with an ejecta mass (Formula presented.), a mass of radioactive (Formula presented.), and an explosion energy (Formula presented.) erg at metallicity (Formula presented.). The SN progenitor radius depends on the adopted distance D to NGC 4151 and its values are (Formula presented.) at D=20 Mpc and (Formula presented.) at D=16 Mpc.