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.
@article{arxiv.0704.0675,
title = {Proto-Neutron Star Winds, Magnetar Birth, and Gamma-Ray Bursts},
author = {B. D. Metzger and T. A. Thompson and E. Quataert},
journal= {arXiv preprint arXiv:0704.0675},
year = {2009}
}
Comments
5 pages; to appear in the AIP conference proceedings of "Supernova 1987A: 20 Years After - Supernovae and Gamma-Ray Bursters", February 19-23, 2007, Aspen, Colorado