Binary star progenitors of long gamma-ray bursts

By Matteo Cantiello, Sung-Chul Yoon, N. Langer, M. Livio. 2007

190 citations recorded by the source corpus.

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 1-D 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 e ffi ciently transport accreted angular momentum into the stellar core. The orbital widening prevents subseq uent tidal synchronization, and the mass gainer rejuvenates and evolves quasi-chemically 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-che mically 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 la rge fraction of long gamma-ray bursts occurs in runaway stars.

Subfields: Astronomy and Astrophysics

View Paper: https://www.semanticscholar.org/paper/fd2969aebf7de266f88a5cdba6880edc3adc9707

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Citations in the corpus

Strongly star forming galaxies in the local Universe with nebular He iiλ4686 emission (2012, background): “This would be the case if some stars rotated fast enough to evolve homogeneously (Maeder 1987; Yoon & Langer 2005; Yoon, Langer & Norman 2006; Cantiello et al. 2007; Meynet & Maeder 2007).”
Stellar population effects on the inferred photon density at reionization (2015, background): “This spin-up of stars by this transfer can result in the rotational mixing of its layers, allowing the more efficient burning of hydrogen in its interior (Cantiello et al. 2007; de Mink et al. 2013).”
The spin of the second-born black hole in coalescing binary black holes (2018, methodology): “In this context, the tidal spin-up of a He-rich star from a compact companion in a close binary system has been investigated in several studies (Brown et al. 2000; Izzard et al. 2004; Petrovic et al. 2005; Cantiello et al. 2007; van den Heuvel & Yoon 2007; Detmers et al. 2008;Eldridge et al.2008).”
Classical Be stars (2013, background): “Another proposed channel to produce long GRBs is via binary evolution (Cantiello et al. 2007), and Tutukov and Fedorova (2007) predict GRB explosion in specific Be binary systems.”
Mass Loss: Its Effect on the Evolution and Fate of High-Mass Stars (2014, background): “The main uncertainties are in the degree to which mass transfer is conservative5 (Cantiello et al. 2007, de Mink et al. 2007), the related question of how the mass gainer responds to the added angular momentum that may lead to critical rotation (de Mink et al. 2013), and the consequent orbital…”
Spectral population synthesis including massive binaries (2009, background): “To our knowledge only the code described by Cantiello et al. (2007) and de Mink et al. (2009) (and references there-in) does so, and is extremely computationally and human input intensive.”
Merging binary black holes formed through chemically homogeneous evolution in short-period stellar binaries (2015, background): “…homogeneous evolution in binary systems High stellar spins can be achieved in binary systems as a result of spin-up by mass accretion (Packet 1981; Cantiello et al. 2007; de Mink et al. 2013) or tidal spinup in very close binary systems (Zahn 1989; Izzard et al. 2004; Detmers et al. 2008; de Mink…”
Formation of Double Neutron Star Systems (2017, background): “…supernova (SN) explosions (Whelan & Iben 1973; Iben & Tutukov 1984; Yoon et al. 2010), possibly including long gamma-ray bursts (GRBs, Woosley 1993; Cantiello et al. 2007), the modelling of accretion processes in X-ray binaries (Lewin & van der Klis 2006) and the formation of mil- email:…”
MODULES FOR EXPERIMENTS IN STELLAR ASTROPHYSICS (MESA): BINARIES, PULSATIONS, AND EXPLOSIONS (2015, background): “On the other hand very few works that include the physics of differential rotation in binaries have been published (Petrovic et al. 2005; Cantiello et al. 2007).”
RECONCILING THE STELLAR AND NEBULAR SPECTRA OF HIGH-REDSHIFT GALAXIES (2016, background): “For example, binary massive stars with metallicities Z∗< 0.004 (Z∗/Z < 0.35) can lead to “quasi-homogeneous evolution” (QHE; Yoon & Langer 2005; Cantiello et al. 2007; Eldridge et al. 2011; Brott et al. 2011; Eldridge & Stanway 2012) in which the more massive star over-flows its Roche lobe and…”
Runaway stars as progenitors of supernovae and gamma-ray bursts (2011, methodology): “While Yoon, Langer & Norman (2006) relate long-duration GRBs to the quasi-chemically homogeneous evolution of rapidlyrotating single stars, we consider only the binary-induced quasi-chemically homogeneous evolution as explored by Cantiello et al. (2007).”
TYPE Ib/c SUPERNOVAE IN BINARY SYSTEMS. I. EVOLUTION AND PROPERTIES OF THE PROGENITOR STARS (2010, methodology): “More recently, Petrovic et al. (2005a) and Cantiello et al. (2007) included the Spruit-Tayler dynamo in their binary models, and discussed possible evolutionary paths of massive binary stars towards long GRBs.”