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Opacity of Ejecta in Calculations of Supernova Light Curves. / Potashov, M. Sh; Blinnikov, S. I.; Sorokina, E. I.

In: Astronomy Letters, Vol. 47, No. 4, 04.2021, p. 204-213.

Research output: Contribution to journal › Article › peer-review

Harvard

Potashov, MS, Blinnikov, SI & Sorokina, EI 2021, 'Opacity of Ejecta in Calculations of Supernova Light Curves', Astronomy Letters, vol. 47, no. 4, pp. 204-213. https://doi.org/10.1134/S1063773721030051

APA

Potashov, M. S., Blinnikov, S. I., & Sorokina, E. I. (2021). Opacity of Ejecta in Calculations of Supernova Light Curves. Astronomy Letters, 47(4), 204-213. https://doi.org/10.1134/S1063773721030051

Vancouver

Potashov MS, Blinnikov SI, Sorokina EI. Opacity of Ejecta in Calculations of Supernova Light Curves. Astronomy Letters. 2021 Apr;47(4):204-213. doi: 10.1134/S1063773721030051

Author

Potashov, M. Sh ; Blinnikov, S. I. ; Sorokina, E. I. / Opacity of Ejecta in Calculations of Supernova Light Curves. In: Astronomy Letters. 2021 ; Vol. 47, No. 4. pp. 204-213.

BibTeX

@article{f51fb52d676a483a997625eea220052d,
title = "Opacity of Ejecta in Calculations of Supernova Light Curves",
abstract = "The plasma opacity in stars depends mainly on the local state of matter (the density, temperature, and chemical composition at the point of interest), but in supernova ejecta it also depends on the expansion velocity gradient, because the Doppler effect shifts the spectral lines differently in different ejecta layers. This effect is known in the literature as the expansion opacity. The existing approaches to the inclusion of this effect, in some cases, predict different results in identical conditions. In this paper we compare the approaches of Blinnikov (1996) and Friend and Castor (1983)–Eastman and Pinto (1993) to calculating the opacity in supernova ejecta and give examples of the influence of different approximations on the model light curves of supernovae.",
keywords = "light curves, opacity, radiative transfer, supernovae",
author = "Potashov, {M. Sh} and Blinnikov, {S. I.} and Sorokina, {E. I.}",
note = "Funding Information: This study was supported by the Russian Foundation for Basic Research (project no. 19-02-00567). Publisher Copyright: {\textcopyright} 2021, Pleiades Publishing, Inc.",
year = "2021",
month = apr,
doi = "10.1134/S1063773721030051",
language = "English",
volume = "47",
pages = "204--213",
journal = "Astronomy Letters",
issn = "1063-7737",
publisher = "Maik Nauka-Interperiodica Publishing",
number = "4",

}

RIS

TY - JOUR

T1 - Opacity of Ejecta in Calculations of Supernova Light Curves

AU - Potashov, M. Sh

AU - Blinnikov, S. I.

AU - Sorokina, E. I.

N1 - Funding Information: This study was supported by the Russian Foundation for Basic Research (project no. 19-02-00567). Publisher Copyright: © 2021, Pleiades Publishing, Inc.

PY - 2021/4

Y1 - 2021/4

N2 - The plasma opacity in stars depends mainly on the local state of matter (the density, temperature, and chemical composition at the point of interest), but in supernova ejecta it also depends on the expansion velocity gradient, because the Doppler effect shifts the spectral lines differently in different ejecta layers. This effect is known in the literature as the expansion opacity. The existing approaches to the inclusion of this effect, in some cases, predict different results in identical conditions. In this paper we compare the approaches of Blinnikov (1996) and Friend and Castor (1983)–Eastman and Pinto (1993) to calculating the opacity in supernova ejecta and give examples of the influence of different approximations on the model light curves of supernovae.

AB - The plasma opacity in stars depends mainly on the local state of matter (the density, temperature, and chemical composition at the point of interest), but in supernova ejecta it also depends on the expansion velocity gradient, because the Doppler effect shifts the spectral lines differently in different ejecta layers. This effect is known in the literature as the expansion opacity. The existing approaches to the inclusion of this effect, in some cases, predict different results in identical conditions. In this paper we compare the approaches of Blinnikov (1996) and Friend and Castor (1983)–Eastman and Pinto (1993) to calculating the opacity in supernova ejecta and give examples of the influence of different approximations on the model light curves of supernovae.

KW - light curves

KW - opacity

KW - radiative transfer

KW - supernovae

UR - http://www.scopus.com/inward/record.url?scp=85111260471&partnerID=8YFLogxK

U2 - 10.1134/S1063773721030051

DO - 10.1134/S1063773721030051

M3 - Article

AN - SCOPUS:85111260471

VL - 47

SP - 204

EP - 213

JO - Astronomy Letters

JF - Astronomy Letters

SN - 1063-7737

IS - 4

ER -

ID: 34174487