proceeding

Proto-Neutron Star Winds, Magnetar Birth, and Gamma-Ray Bursts

Brian D. MetzgerbDepartment of Physics, 366 LeConte Hall, University of California, Berkeley, CA 94720Todd A. ThompsonAstronomy Department and Theoretical Astrophysics Center , 601 Campbell Hall , Berkeley , CA 94720 ;Eliot QuataertDepartment of Astrophysical Sciences , Peyton Hall-Ivy Lane , Princeton University , Princeton , NJ 08544 ;S. ImmlerK. W. Weiler

2007en

ABI

Annotatsiya

We begin by reviewing the theory of thermal, neutrino‐driven proto‐neutron star (PNS) winds. Including the effects of magnetic fields and rotation, we then derive the mass and energy loss from magnetically‐driven PNS winds for both relativistic and non‐relativistic outflows, including important multi‐dimensional considerations. With these simple analytic scalings we argue that proto‐magnetars born with ∼ millisecond rotation periods produce relativistic winds just a few seconds after core collapse with luminosities, timescales, mass‐loading, and internal shock efficiencies favorable for producing long‐duration gamma‐ray bursts.

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Identifikatorlar

DOI: 10.1063/1.3682954

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