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Бакланов, Петр Валерьевич

Организационные подразделения

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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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Бакланов

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Петр Валерьевич

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Теперь показываю 1 - 10 из 11

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A 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
Только метаданные
Strongly Lensed Supernova Refsdal: Refining Time Delays Based on the Supernova Explosion Models
(2021) Baklanov, P.; Lyskova, N.; Blinnikov, S.; Nomoto, K.; Бакланов, Петр Валерьевич
We 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.
Только метаданные
On 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
Только метаданные
SN 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
Только метаданные
Type 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.
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SN 2018hna: 1987A-like Supernova with a Signature of Shock Breakout
(2019) Singh, Avinash; Sahu, D. K.; Anupama, G. C.; Kumar, Brajesh; Baklanov, Petr V.; Бакланов, Петр Валерьевич
High-cadence ultraviolet, optical, and near-infrared photometric and low-resolution spectroscopic observations of the peculiar Type II supernova (SN) 2018hna are presented. The early-phase multiband light curves (LCs) exhibit the adiabatic cooling envelope emission following the shock breakout up to similar to 14 days from the explosion. SN. 2018hna has a rise time of similar to 88 days in the V band, similar to SN 1987A. A Ni-56 mass of similar to 0.087 +/- 0.004 M-circle dot is inferred for SN 2018hna from its bolometric LC. Hydrodynamical modeling of the cooling phase suggests a progenitor with a radius similar to 50 R-circle dot, a mass of similar to 14-20 M-circle dot, and an explosion energy of similar to 1.7-2.9 x 10(51) erg. The smaller inferred radius of the progenitor than a standard red supergiant is indicative of a blue supergiant progenitor of SN 2018hna. A subsolar metallicity (similar to 0.3 Z(circle dot)) is inferred for the host galaxy UGC 07534, concurrent with the low-metallicity environments of 1987A-like events.
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The influence of line opacity treatment in STELLA on supernova light curves
(2020) Kozyreva, A.; Shingles, L.; Mironov, A.; Blinnikov, S.; Baklanov, P.; Бакланов, Петр Валерьевич
© 2020 The Author(s)We systematically explore the effect of the treatment of line opacity on supernova light curves. We find that it is important to consider line opacity for both scattering and absorption (i.e. thermalization, which mimics the effect of fluorescence). We explore the impact of the degree of thermalization on three major types of supernovae: Type Ia, Type II-peculiar, and Type II-plateau. For this we use the radiative transfer code STELLA and analyse broad-band light curves in the context of simulations done with the spectral synthesis code ARTIS and in the context of a few examples of observed supernovae of each type. We found that the plausible range for the ratio between absorption and scattering in the radiation hydrodynamics code STELLA is (0.8-1):(0.2-0), i.e. the recommended thermalization parameter is 0.9.
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Parameters of the type-IIP supernova SN 2012aw
(2021) Nikiforova, A. A.; Blinnikov, S. I.; Blinov, D. A.; Grishina, T. S.; Baklanov, P. V.; Бакланов, Петр Валерьевич
© 2021 The Author(s) Published by Oxford University Press on behalf of Royal Astronomical Society.We present the results the photometric observations of the Type IIP supernova SN 2012aw obtained for the time interval from 7 to 371 d after the explosion. Using the previously published values of the photospheric velocities, we have computed the hydrodynamic model which simultaneously reproduced the photometry observations and velocity measurements. We found the parameters of the pre-supernova: radius R = 500 R, nickel mass M(56Ni$)\, \sim 0.06\, \rm M_\odot$, pre-supernova mass 25 M, mass of ejected envelope 23.6 M, explosion energy E ∼2 × 1051 erg. The model progenitor mass M = 25 M significantly exceeds the upper limit mass M = 17 M, obtained from analysis the pre-SNe observations. This result confirms once more that the 'Red Supergiant Problem' must be resolved by stellar evolution and supernova explosion theories in interaction with observations.
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Supernova 2018aoq and a distance to Seyfert galaxy NGC 4151
(2019) Tsvetkov, D. Y.; Potashov, M. S.; Oknyansky, V. L.; Mikailov, K. M.; Baklanov, P. V.; Бакланов, Петр Валерьевич
© 2019 The Author(s) Published by Oxford University Press on behalf of the Royal Astronomical Society.We present optical photometric observations of SN 2018aoq from 2 to 100 d after explosion, and 7 spectra at epochs from 11 to 71 d. The light curves and spectra are typical for SNe II-P. As previously reported, SN 2018aoq appears to be of intermediate brightness between subluminous and normal SNe II-P. SN 2018aoq was discovered in Seyfert galaxy NGC 4151, for which the distance is uncertain. We utilized the expanding photosphere method using three sets of filter combinations and velocities derived from the absorption minima of Fe ii lines and obtained a distance of 20.0 ± 1.6 Mpc. The standard candle method applied to SN 2018aoq yields a distance of 16.6 ± 1.1 Mpc. Both values are consistent with the distance measurements for NGC 4151 based on geometric method.
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Synthetic observables for electron-capture supernovae and low-mass core collapse supernovae
(2021) Kozyreva, A.; Jones, S.; Stockinger, G.; Janka, H. -T.; Baklanov, P.; Бакланов, Петр Валерьевич
© 2021 The Author(s) Published by Oxford University Press on behalf of Royal Astronomical Society.Stars in the mass range from 8 M· to 10 M· are expected to produce one of two types of supernovae (SNe), either electron-capture supernovae (ECSNe) or core-collapse supernovae (CCSNe), depending on their previous evolution. Either of the associated progenitors retain extended and massive hydrogen-rich envelopes and the observables of these SNe are, therefore, expected to be similar. In this study, we explore the differences in these two types of SNe. Specifically, we investigate three different progenitor models: a solar-metallicity ECSN progenitor with an initial mass of 8.8 M·, a zero-metallicity progenitor with 9.6 M·, and a solar-metallicity progenitor with 9 M·, carrying out radiative transfer simulations for these progenitors. We present the resulting light curves for these models. The models exhibit very low photospheric velocity variations of about 2000 km s-1; therefore, this may serve as a convenient indicator of low-mass SNe. The ECSN has very unique light curves in broad-bands, especially the U band, and does not resemble any currently observed SN. This ECSN progenitor being part of a binary will lose its envelope for which reason the light curve becomes short and undetectable. The SN from the 9.6 M· progenitor exhibits also quite an unusual light curve, explained by the absence of metals in the initial composition. The artificially iron-polluted 9.6 M· model demonstrates light curves closer to normal SNe IIP. The SN from the 9 M· progenitor remains the best candidate for so-called low-luminosity SNe IIP like SN 1999br and SN 2005cs.