Presupernova evolution in massive interacting binaries

Podsiadlowski, Ph.; Joss, P. C.; Hsu, Jonathan Y.

doi:10.1086/171341

Cited by 696 publications

(765 citation statements)

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“…Most Type Ib/Ic SNe are expected to originate in binary systems from the initially more massive star which has lost its hydrogen envelope by mass-transfer to its companion (Podsiadlowski et al 1992;Eldridge et al 2008); these pre-SN stars typically have an envelope mass of 1 M⊙ or more (Yoon et al 2010). In close X-ray binaries, however, a second mass-transfer stage from a helium star to a NS can strip the helium star further prior to the SN (Habets 1986;Dewi et al 2002;Dewi & Pols 2003;Ivanova et al 2003;Tauris et al 2013, and references therein).…”

Section: Introductionmentioning

confidence: 99%

Ultra-stripped supernovae: progenitors and fate

Tauris¹,

Langer²,

Podsiadlowski³

2015

Monthly Notices of the Royal Astronomical Society

406

613

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The explosion of ultra-stripped stars in close binaries can lead to ejecta masses < 0.1 M ⊙ and may explain some of the recent discoveries of weak and fast optical transients. In Tau ris et al. (2013), it was demonstrated that helium star companions to neutron stars (NSs) may experience mass transfer and evolve into naked ∼ 1.5 M ⊙ metal cores, barely above the Chandrasekhar mass limit. Here we elaborate on this work and present a systematic investigation of the progenitor evolution leading to ultra-stripped supernovae (SNe). In particular, we examine the binary parameter space leading to electron-capture (EC SNe) and iron core-collapse SNe (Fe CCSNe), respectively, and determine the amount of helium ejected with applications to their observational classification as Type Ib or Type Ic. We mainly evolve systems where the SN progenitors are helium star donors of initial mass M He = 2.5 − 3.5 M ⊙ in tight binaries with orbital periods of P orb = 0.06 − 2.0 days, and hosting an accreting NS, but we also discuss the evolution of wider systems and of both more massive and lighter -as well as single -helium stars. In some cases we are able to follow the evolution until the onset of silicon burning, just a few days prior to the SN explosion. We find that ultra-stripped SNe are possible for both EC SNe and Fe CCSNe. EC SNe only occur for M He = 2.60 − 2.95 M ⊙ depending on P orb . The general outcome, however, is an Fe CCSN above this mass interval and an ONeMg or CO white dwarf for smaller masses. For the exploding stars, the amount of helium ejected is correlated with P orb -the tightest systems even having donors being stripped down to envelopes of less than 0.01 M ⊙ . We estimate the rise time of ultra-stripped SNe to be in the range 12 hr − 8 days, and light curve decay times between 1 and 50 days. A number of fitting formulae for our models are provided with applications to population synthesis. Ultrastripped SNe may produce NSs in the mass range 1.10 − 1.80 M ⊙ and are highly relevant for LIGO/VIRGO since most (possibly all) merging double NS systems have evolved through this phase. Finally, we discuss the low-velocity kicks which might be imparted on these resulting NSs at birth.

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Section: Introductionmentioning

confidence: 99%

Ultra-stripped supernovae: progenitors and fate

Tauris¹,

Langer²,

Podsiadlowski³

2015

Monthly Notices of the Royal Astronomical Society

406

613

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“…While we provide only one example, it seems likely that this scenario applies to most massive close binary components which accrete or gain an appreciable amount of mass; this may encompass Case A binaries and early Case B binaries (Podsiadlowski et al 1992;Wellstein & Langer 1999;. Case A merger are also likely contributing to this scenario.…”

Section: Discussionmentioning

confidence: 97%

“…However, massive close binary evolution enhances the IRF to what we may call the apparent IRF as measured by Mokiem et al (2006), which leads to the redshift dependent GRB rate as worked out by Yoon et al (2006). According to the binary population synthesis model of Podsiadlowski et al (1992), about 10% of all massive binaries might lead to a Case A merger or early Case B mass transfer, which is sufficient to populate the rapidly rotating part of the IRF of Mokiem et al In that context, the rapidly rotating O star in the sample of Mokiem et al (2006) which does not appear as runaway star could either have an undetected high proper motion, or it could be the result of a Case A merger -where no runaway is produced.…”

Section: Binaries and The Distribution Of Rotational Velocitiesmentioning

confidence: 98%

Binary star progenitors of long gamma-ray bursts

Cantiello

Yoon

Langer

et al. 2007

A&A

211

250

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Context. The collapsar model for long gamma-ray bursts requires a rapidly rotating Wolf-Rayet star as progenitor. Aims. We test the idea of producing rapidly rotating Wolf-Rayet stars in massive close binaries through mass accretion and consecutive quasi-chemically homogeneous evolution -the latter had previously been shown to provide collapsars below a certain metallicity threshold. Methods. We use a 1D hydrodynamic binary evolution code to simulate the evolution of a 16 + 15 M binary model with an initial orbital period of 5 days and SMC metallicity (Z = 0.004). Internal differential rotation, rotationally induced mixing and magnetic fields are included in both components, as well as non-conservative mass and angular momentum transfer, and tidal spin-orbit coupling. Results. The considered binary system undergoes early Case B mass transfer. The mass donor becomes a helium star and dies as a type Ib/c supernova. The mass gainer is spun-up, and internal magnetic fields efficiently transport accreted angular momentum into the stellar core. The orbital widening prevents subsequent tidal synchronization, and the mass gainer rejuvenates and evolves quasichemically homogeneously thereafter. The mass donor explodes 7 Myr before the collapse of the mass gainer. Assuming the binary to be broken-up by the supernova kick, the potential gamma-ray burst progenitor would become a runaway star with a space velocity of 27 km s −1 , traveling about 200 pc during its remaining lifetime. Conclusions. The binary channel presented here does not, as such, provide a new physical model for collapsar production, as the resulting stellar models are almost identical to quasi-chemically homogeneously evolving rapidly rotating single stars. However, it may provide a means for massive stars to obtain the required high rotation rates. Moreover, it suggests that a possibly large fraction of long gamma-ray bursts occurs in runaway stars.

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“…Heger et al 2003); (2) lower mass binaries stripped through interaction by a close companion (e.g. Podsiadlowski, Joss & Hsu 1992). Therefore, the progenitors of SN Ibc 1 may be more massive than those of normal SN II (8 − 16 M⊙; Smartt 2009) or explode in regions of higher metallicity (e.g.…”

Section: Introductionmentioning

confidence: 99%

Supernovae and their host galaxies – II. The relative frequencies of supernovae types in spirals

Hakobyan¹,

Nazaryan²,

Adibekyan³

et al. 2014

Monthly Notices of the Royal Astronomical Society

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We present an analysis of the relative frequencies of different supernova (SN) types in spirals with various morphologies and in barred or unbarred galaxies. We use a well-defined and homogeneous sample of spiral host galaxies of 692 SNe from the Sloan Digital Sky Survey in different stages of galaxy-galaxy interaction and activity classes of nucleus. We propose that the underlying mechanisms shaping the number ratios of SNe types can be interpreted within the framework of interaction-induced star formation, in addition to the known relations between morphologies and stellar populations. We find a strong trend in behaviour of the N Ia /N CC ratio depending on host morphology, such that early spirals include more Type Ia SNe. The N Ibc /N II ratio is higher in a broad bin of early-type hosts. The N Ia /N CC ratio is nearly constant when changing from normal, perturbed to interacting galaxies, then declines in merging galaxies, whereas it jumps to the highest value in post-merging/remnant galaxies. In contrast, the N Ibc /N II ratio jumps to the highest value in merging galaxies and slightly declines in post-merging/remnant subsample. The interpretation is that the star formation rates and morphologies of galaxies, which are strongly affected in the final stages of interaction, have an impact on the number ratios of SNe types. The N Ia /N CC (N Ibc /N II ) ratio increases (decreases) from star-forming to active galactic nuclei (AGN) classes of galaxies. These variations are consistent with the scenario of an interaction-triggered starburst evolving into AGN during the later stages of interaction, accompanied with the change of star formation and transformation of the galaxy morphology into an earlier type.

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Presupernova evolution in massive interacting binaries

Cited by 696 publications

References 0 publications

Ultra-stripped supernovae: progenitors and fate

Ultra-stripped supernovae: progenitors and fate

Binary star progenitors of long gamma-ray bursts

Supernovae and their host galaxies – II. The relative frequencies of supernovae types in spirals

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