Supernovae in colliding-wind binaries: observational signatures in the first year
The result's identifiers
Result code in 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>
Alternative codes found
RIV/00216224:14310/22:00125049
Result on the web
<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>
Alternative languages
Result language
angličtina
Original language name
Supernovae in colliding-wind binaries: observational signatures in the first year
Original language description
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 << 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.
Czech name
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Czech description
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Classification
Type
J<sub>imp</sub> - Article in a specialist periodical, which is included in the Web of Science database
CEP classification
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OECD FORD branch
10308 - Astronomy (including astrophysics,space science)
Result continuities
Project
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Continuities
R - Projekt Ramcoveho programu EK
Others
Publication year
2022
Confidentiality
S - Úplné a pravdivé údaje o projektu nepodléhají ochraně podle zvláštních právních předpisů
Data specific for result type
Name of the periodical
Monthly Notices of the Royal Astronomical Society
ISSN
0035-8711
e-ISSN
1365-2966
Volume of the periodical
510
Issue of the periodical within the volume
3
Country of publishing house
GB - UNITED KINGDOM
Number of pages
15
Pages from-to
3276-3290
UT code for WoS article
000749577000010
EID of the result in the Scopus database
2-s2.0-85134141365