Simulations of stripped core-collapse supernovae in close binaries

Rimoldi, A.J.; Zwart, Simon Portegies; Rossi, Elena M.

doi:10.1186/s40668-016-0015-4

Cited by 35 publications

(38 citation statements)

References 75 publications

(129 reference statements)

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“…Similar distributions can be derived for all our parameter variations from the data files that will be made available. These distributions can inform studies of the interaction of the SN shock with the companion star (e.g., Wheeler et al 1975;Liu et al 2015;Rimoldi et al 2016;Hirai et al 2018). We show in Fig.…”

Section: Appendix B: Output Filesmentioning

confidence: 80%

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Massive runaway and walkaway stars

Renzo

Zapartas

Mink

et al. 2019

A&A

214

259

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We perform an extensive numerical study of the evolution of massive binary systems to predict the peculiar velocities that stars obtain when their companion collapses and disrupts the system. Our aim is to (i) identify which predictions are robust against model uncertainties and assess their implications, (ii) investigate which physical processes leave a clear imprint and may therefore be constrained observationally, and (iii) provide a suite of publicly available model predictions to allow for the use of kinematic constraints from the Gaia mission. We find that 22+26−8% of all massive binary systems merge prior to the first core-collapse in the system. Of the remainder, 86+11−9% become unbound because of the core-collapse. Remarkably, this rarely produces runaway stars (observationally defined as stars with velocities above 30 km s−1). These are outnumbered by more than an order of magnitude by slower unbound companions, or “walkaway stars”. This is a robust outcome of our simulations and is due to the reversal of the mass ratio prior to the explosion and widening of the orbit, as we show analytically and numerically. For stars more massive than 15 M⊙, we estimate that 10+5−8% are walkaways and only 0.5+1.0−0.4% are runaways, nearly all of which have accreted mass from their companion. Our findings are consistent with earlier studies; however, the low runaway fraction we find is in tension with observed fractions of about 10%. Thus, astrometric data on presently single massive stars can potentially constrain the physics of massive binary evolution. Finally, we show that the high end of the mass distributions of runaway stars is very sensitive to the assumed black hole natal kicks, and we propose this as a potentially stringent test for the explosion mechanism. We also discuss companions remaining bound that can evolve into X-ray and gravitational wave sources.

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Section: Appendix B: Output Filesmentioning

confidence: 80%

“…ii) The SN shock can interact with the companion star. (e.g., Wheeler et al 1975;Liu et al 2015;Rimoldi et al 2016;Hirai et al 2018). The shock can dynamically remove mass from the companion (stripping), heat the envelope of the secondary, thus enhancing its own mass loss (ablation), and deposit mass and momentum on the secondary.…”

Section: Natal Kickmentioning

confidence: 99%

Massive runaway and walkaway stars

Renzo

Zapartas

Mink

et al. 2019

A&A

214

259

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“…compositions and velocities) is usually small (e.g. Hirai et al, 2014;Kalogera, 1996;Liu et al, 2015b;Rimoldi et al, 2015), unless the pre-supernova separation between the stars is smaller than a few solar radii. For this reason, we assume the dynamics of the companion stars are not affected by the expanding shell of material, and the companion stars neither accrete nor are stripped of mass.…”

Section: Supernova Explosions In Tresmentioning

confidence: 99%

The evolution of hierarchical triple star-systems

2016

Self Cite

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Field stars are frequently formed in pairs, and many of these binaries are part of triples or even higher-order systems. Even though, the principles of single stellar evolution and binary evolution, have been accepted for a long time, the long-term evolution of stellar triples is poorly understood. The presence of a third star in an orbit around a binary system can significantly alter the evolution of those stars and the binary system. The rich dynamical behaviour in three-body systems can give rise to Lidov-Kozai cycles, in which the eccentricity of the inner orbit and the inclination between the inner and outer orbit vary periodically. In turn, this can lead to an enhancement of tidal effects (tidal friction), gravitational-wave emission and stellar interactions such as mass transfer and collisions. The lack of a self-consistent treatment of triple evolution, including both three-body dynamics as well as stellar evolution, hinders the systematic study and general understanding of the long-term evolution of triple systems. In this paper, we aim to address some of these hiatus, by discussing the dominant physical processes of hierarchical triple evolution, and presenting heuristic recipes for these processes. To improve our understanding on hierarchical stellar triples, these descriptions are implemented in a public source code TrES, which combines three-body dynamics (based on the secular approach) with stellar evolution and their mutual influences. Note that modelling through a phase of stable mass transfer in an eccentric orbit is currently not implemented in TrES, but can be implemented with the appropriate methodology at a later stage.

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“…If the core-collapse produces a successful explosion, the newly "widowed star" will be hit by the blast wave (e.g., Moriya et al, 2015;Hirai et al, 2018), which can alter its appearance for a few thermal timescales by depositing energy in the star and removing some mass, although the latter effect is typically small (e.g. Liu et al, 2015;Rimoldi et al, 2016).…”

Section: How Explosions Can Affect Binariesmentioning

confidence: 99%

The explosive life of massive binaries

Renzo¹,

Zapartas²

2020

caosp

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Massive stars are born predominantly as members of binary (or higher multiplicity) systems, and the presence of a companion can significantly alter their life and final fate. Therefore, any observed sample of massive stars or associated transients is likely to be significantly influenced by the effects of binarity. Here, we focus on the relationship between massive binary evolution and core-collapse supernova events. In the vast majority of the cases, the first core-collapse event happening in a binary system unbinds the two stars. Studying the population of companion stars, either at the supernova site, or as "widowed" stars long after the explosion, can be used to constrain the previous orbital evolution of the binary progenitor, and explosion physics of their former companion. Specifically, the population of "widowed" stars might provide statistical constraints on the typical amplitude of black hole natal kicks without seeing neither the black holes nor the transient possibly associated to their formation. Binarity also has a large impact on the predicted population of supernova sub-types, including hydrogen-rich type II supernovae, with a significant fraction of hydrogen-rich stars at explosions being either merger products or accretors.

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Simulations of stripped core-collapse supernovae in close binaries

Cited by 35 publications

References 75 publications

Massive runaway and walkaway stars

Massive runaway and walkaway stars

The evolution of hierarchical triple star-systems

The explosive life of massive binaries

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