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  Compact Binary Progenitors of Short Gamma-Ray Bursts

Giacomazzo, B., Perna, R., Rezzolla, L., Troja, E., & Lazzati, D. (2013). Compact Binary Progenitors of Short Gamma-Ray Bursts. The Astrophysical Journal Letters, 762: L18. doi:10.1088/2041-8205/762/2/L18.

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Item Permalink: http://hdl.handle.net/11858/00-001M-0000-000E-EEB7-2 Version Permalink: http://hdl.handle.net/11858/00-001M-0000-000E-EEB8-F
Genre: Journal Article

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1210.8152 (Preprint), 252KB
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Giacomazzo, Bruno1, Author              
Perna, Rosalba, Author
Rezzolla, Luciano1, Author              
Troja, Eleonora, Author
Lazzati, Davide, Author
Affiliations:
1Astrophysical Relativity, AEI-Golm, MPI for Gravitational Physics, Max Planck Society, ou_24013              

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Free keywords: Astrophysics, High Energy Astrophysical Phenomena, astro-ph.HE,General Relativity and Quantum Cosmology, gr-qc
 Abstract: In recent years, detailed observations and accurate numerical simulations have provided support to the idea that mergers of compact binaries containing either two neutron stars (NSs) or an NS and a black hole (BH) may constitute the central engine of short gamma-ray bursts (SGRBs). The merger of such compact binaries is expected to lead to the production of a spinning BH surrounded by an accreting torus. Several mechanisms can extract energy from this system and power the SGRBs. Here we connect observations and numerical simulations of compact binary mergers, and use the current sample of SGRBs with measured energies to constrain the mass of their powering tori. By comparing the masses of the tori with the results of fully general-relativistic simulations, we are able to infer the properties of the binary progenitors which yield SGRBs. By assuming a constant efficiency in converting torus mass into jet energy, epsilon_{jet}=10%, we find that most of the tori have masses smaller than 0.01M_{sun}, favoring "high-mass" binary NSs mergers, i.e., binaries with total masses >~1.5 the maximum mass of an isolated NS. This has important consequences for the gravitational-wave signals that may be detected in association with SGRBs, since "high-mass" systems do not form a long-lived hypermassive NS after the merger. While NS-BH systems cannot be excluded to be the engine of at least some of the SGRBs, the BH would need to have an initial spin of ~0.9, or higher.

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 Dates: 2012-10-302012-12-112013
 Publication Status: Published in print
 Pages: 6 pages, 3 figures. Extended the discussion on jet efficiency. Accepted for publication on The Astrophysical Journal Letters
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 Identifiers: arXiv: 1210.8152
DOI: 10.1088/2041-8205/762/2/L18
URI: http://arxiv.org/abs/1210.8152
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Title: The Astrophysical Journal Letters
  Other : Astrophys. J. Lett.
Source Genre: Journal
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Publ. Info: Chicago, IL : University of Chicago Press for the American Astronomical Society
Pages: - Volume / Issue: 762 Sequence Number: L18 Start / End Page: - Identifier: ISSN: 0004-637X
CoNE: /journals/resource/954922828215