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Title:
Binary star progenitors of long gamma-ray bursts
Authors:
Cantiello, M.; Yoon, S.-C.; Langer, N.; Livio, M.
Affiliation:
AA(Institute for Astronomy (IfA)Astronomical Institute, Utrecht University, Princetonplein 5, 3584 CC Utrecht, The Netherlands ), AB(Astronomical Institute Anton Pannekoek, University of Amsterdam, Kruislaan 403, 1098 SJ Amsterdam, The Netherlands ), AC(Institute for Astronomy (IfA)Astronomical Institute, Utrecht University, Princetonplein 5, 3584 CC Utrecht, The Netherlands), AD(Space Telescope Science Institute, 3700 San Martin Drive, Baltimore, MD 21218, USA)
Publication:
Astronomy and Astrophysics, Volume 465, Issue 2, April II 2007, pp.L29-L33 (A&A Homepage)
Publication Date:
04/2007
Origin:
EDP Sciences
Keywords:
stars: binaries: general, stars: rotation, stars: evolution, stars: mass-loss, supernovae: general, gamma rays: bursts
DOI:
10.1051/0004-6361:20077115
Bibliographic Code:
2007A&A...465L..29C

Abstract

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 Mȯ 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 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-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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