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.
- ПубликацияОткрытый доступThe 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.
- ПубликацияОткрытый доступSynthetic 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.
- ПубликацияОткрытый доступShock breakouts from red supergiants: analytical and numerical predictions(2020) Kozyreva, A.; Nakar, E.; Waldman, R.; Blinnikov, S.; Baklanov, P.; Бакланов, Петр ВалерьевичThe signal from a shock breakout (SBO) is the first signature of a supernova explosion, apart from gravitational waves and neutrinos. Observational properties of SBOs, such as bolometric luminosity and colour temperature, are connected with the parameters of the supernova progenitor and explosion. The detection of SBOs or the cooling of SBOs will constrain the progenitor and explosion models of collapsing stars. Since the recent launch of the eROSITA on the SPECTRUM-RG spacecraft, the detection rate for SBOs is a few events per year. In the current study, we examine the analytical formulae derived by Shussman, Waldman & Nakar (arXiv:1610.05323). We use four red supergiant models from their study, while running explosions with the radiation hydrodynamics code STELLA. We conclude that there is a good agreement between analytical and numerical approaches for bolometric luminosity and colour temperature during SBOs. The analytical formulae for the SBO signal based on the global supernova parameters can be used instead of running time-consuming numerical simulations. We define the spectral range in which analytical formulae for SBO spectra are valid. We provide an improved analytical expression for the SBO spectral energy distribution. We confirm that the colour temperature is dependent on radius derived by analytical studies and we suggest using early time observations to confine the progenitor radius. Additionally, we show the prediction for the SBO signal from red supergiants as seen by eROSITA.