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@article{1803639, author = {Pejcha, Ondřej and Calderón, Diego and Kurfürst, Petr}, article_number = {3}, doi = {http://dx.doi.org/10.1093/mnras/stab3729}, keywords = {binaries: general; stars: massive; supernovae: general; stars: winds; outflows}, language = {eng}, issn = {0035-8711}, journal = {Monthly Notices of the Royal Astronomical Society}, title = {Supernovae in colliding-wind binaries: observational signatures in the first year}, url = {https://doi.org/10.1093/mnras/stab3729}, volume = {510}, year = {2022} }
TY - JOUR ID - 1803639 AU - Pejcha, Ondřej - Calderón, Diego - Kurfürst, Petr PY - 2022 TI - Supernovae in colliding-wind binaries: observational signatures in the first year JF - Monthly Notices of the Royal Astronomical Society VL - 510 IS - 3 SP - 3276-3290 EP - 3276-3290 PB - Oxford University Press SN - 00358711 KW - binaries: general KW - stars: massive KW - supernovae: general KW - stars: winds KW - outflows UR - https://doi.org/10.1093/mnras/stab3729 N2 - When a core-collapse supernova 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 supernova 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 supernova 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 supernova luminosity only for double red supergiant binaries with mass ratios q less than 0.9, wind mass-loss rates greater than 10^{-4} solar mass per year, and separations between about 50 and 1500 AU. The required mass-loss rate increases for binaries with smaller q or primaries with faster wind. We estimate that much less than 1 percent 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. ER -
PEJCHA, Ondřej, Diego CALDERÓN a Petr KURFÜRST. Supernovae in colliding-wind binaries: observational signatures in the first year. \textit{Monthly Notices of the Royal Astronomical Society}. Oxford University Press, 2022, roč.~510, č.~3, s.~3276-3290. ISSN~0035-8711. Dostupné z: https://dx.doi.org/10.1093/mnras/stab3729.
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