Supernovae in colliding-wind binaries: observational signatures in the first year

Kód výsledku v IS VaVaI

<a href="https://www.isvavai.cz/riv?ss=detail&h=RIV%2F00216208%3A11320%2F22%3A10456323" target="_blank" >RIV/00216208:11320/22:10456323 - isvavai.cz</a>

Nalezeny alternativní kódy

RIV/00216224:14310/22:00125049

Výsledek na webu

<a href="https://verso.is.cuni.cz/pub/verso.fpl?fname=obd_publikace_handle&handle=rZWXxy~Olc" target="_blank" >https://verso.is.cuni.cz/pub/verso.fpl?fname=obd_publikace_handle&handle=rZWXxy~Olc</a>

DOI - Digital Object Identifier

<a href="http://dx.doi.org/10.1093/mnras/stab3729" target="_blank" >10.1093/mnras/stab3729</a>

Jazyk výsledku

angličtina

Název v původním jazyce

Supernovae in colliding-wind binaries: observational signatures in the first year

Popis výsledku v původním jazyce

When a core-collapse supernova (SN) explodes in a binary star system, the ejecta might encounter an overdense shell, where the stellar winds of the two stars previously collided. In this work, we investigate effects of such interactions on SN light curves on time-scales from the early flash ionization signatures to approximately one year after the explosion. We construct a model of the colliding-wind shell in an orbiting binary star system and we provide an analytical expression for the shell thickness and density, which we calibrate with three-dimensional adaptive mesh refinement hydrodynamical simulations probing different ratios of wind momenta and different regimes of radiative cooling efficiency. We model the angle-dependent interaction of SN ejecta with the circumstellar medium and estimate the shock radiative efficiency with a realistic cooling function. We find that the radiated shock power exceeds typical Type IIP SN luminosity only for double red supergiant binaries with mass ratios q greater than or similar to 0.9, wind mass-loss rates (M) over dot greater than or similar to 10(-4) M-circle dot yr(-1), and separations between about 50 and 1500 au. The required (M) over dot increases for binaries with smaller q or primaries with faster wind. We estimate that &lt;&lt; 1 per cent of all collapsing massive stars satisfy the conditions on binary mass ratio and separation. Recombination luminosities due to colliding wind shells are at most a factor of 10 higher than for an otherwise unperturbed constant-velocity wind, but higher densities associated with wind acceleration close to the star provide much stronger signal.

Název v anglickém jazyce

Supernovae in colliding-wind binaries: observational signatures in the first year

Popis výsledku anglicky

When a core-collapse supernova (SN) explodes in a binary star system, the ejecta might encounter an overdense shell, where the stellar winds of the two stars previously collided. In this work, we investigate effects of such interactions on SN light curves on time-scales from the early flash ionization signatures to approximately one year after the explosion. We construct a model of the colliding-wind shell in an orbiting binary star system and we provide an analytical expression for the shell thickness and density, which we calibrate with three-dimensional adaptive mesh refinement hydrodynamical simulations probing different ratios of wind momenta and different regimes of radiative cooling efficiency. We model the angle-dependent interaction of SN ejecta with the circumstellar medium and estimate the shock radiative efficiency with a realistic cooling function. We find that the radiated shock power exceeds typical Type IIP SN luminosity only for double red supergiant binaries with mass ratios q greater than or similar to 0.9, wind mass-loss rates (M) over dot greater than or similar to 10(-4) M-circle dot yr(-1), and separations between about 50 and 1500 au. The required (M) over dot increases for binaries with smaller q or primaries with faster wind. We estimate that &lt;&lt; 1 per cent of all collapsing massive stars satisfy the conditions on binary mass ratio and separation. Recombination luminosities due to colliding wind shells are at most a factor of 10 higher than for an otherwise unperturbed constant-velocity wind, but higher densities associated with wind acceleration close to the star provide much stronger signal.

Druh

J_imp - Článek v periodiku v databázi Web of Science

CEP obor

—

OECD FORD obor

10308 - Astronomy (including astrophysics,space science)

Projekt

—

Návaznosti

R - Projekt Ramcoveho programu EK

Rok uplatnění

2022

Kód důvěrnosti údajů

S - Úplné a pravdivé údaje o projektu nepodléhají ochraně podle zvláštních právních předpisů

Název periodika

Monthly Notices of the Royal Astronomical Society

ISSN

0035-8711

e-ISSN

1365-2966

Svazek periodika

510

Číslo periodika v rámci svazku

3

Stát vydavatele periodika

GB - Spojené království Velké Británie a Severního Irska

Počet stran výsledku

15

Strana od-do

3276-3290

Kód UT WoS článku

000749577000010

EID výsledku v databázi Scopus

2-s2.0-85134141365