Journal Article

Time-dependent models of accretion discs formed from compact object mergers

B. D. Metzger, A. L. Piro and E. Quataert

in Monthly Notices of the Royal Astronomical Society

Published on behalf of The Royal Astronomical Society

Volume 390, issue 2, pages 781-797
Published in print October 2008 | ISSN: 0035-8711
Published online October 2008 | e-ISSN: 1365-2966 | DOI: http://dx.doi.org/10.1111/j.1365-2966.2008.13789.x
Time-dependent models of accretion discs formed from compact object mergers

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We present time-dependent models of the remnant accretion discs created during compact object mergers, focusing on the energy available from accretion at late times and the composition of the disc and its outflows. We calculate the dynamics near the outer edge of the disc, which contains the majority of the disc's mass and determines the accretion rate on to the central black hole. This treatment allows us to follow the evolution over much longer time-scales (100 s or longer) than current hydrodynamic simulations. At late times the disc becomes advective and its properties asymptote to self-similar solutions with an accretion rate (neglecting outflows). This late-time accretion can in principle provide sufficient energy to power the late-time activity observed by Swift from some short-duration gamma-ray bursts. However, because outflows during the advective phase unbind the majority of the remaining mass, it is difficult for the remnant disc alone to produce significant accretion power well beyond the onset of the advective phase. Unless the viscosity is quite low (α≲ 10−3), this occurs before the start of observed flaring at ∼30 s; continued mass inflow at late times thus appears required to explain the late-time activity from short-duration gamma-ray bursts. We show that the composition of the disc freezes-out when the disc is relatively neutron rich (electron fraction Ye≃ 0.3). Roughly 10−2M⊙ of this neutron-rich material is ejected by winds at late times. During earlier, neutrino-cooled phases of accretion, neutrino irradiation of the disc produces a wind with Ye≃ 0.5, which synthesizes at most ∼10−3M⊙ of 56Ni. We highlight what conditions are favorable for 56Ni production and predict, in the best cases, optical and infrared transients peaking ∼0.5–2 d after the burst, with fluxes a factor of ∼10 below the current observational limits.

Keywords: accretion, accretion discs; black hole physics; neutrinos; gamma-rays: bursts

Journal Article.  13392 words.  Illustrated.

Subjects: Astronomy and Astrophysics

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