Acceleration of GRB outflows by Poynting flux dissipation
Max-Planck-Institut für Astrophysik, Postfach 1317, 85741 Garching bei München, Germany
Corresponding author: email@example.com
Accepted: 11 March 2002
We study magnetically powered relativistic outflows in which a part of the magnetic energy is dissipated internally by reconnection. For GRB parameters, and assuming that the reconnection speed scales with the Alfvén speed, significant dissipation can take place both inside and outside the photosphere of the flow. The process leads to a steady increase of the flow Lorentz factor with radius. With an analytic model we show how the efficiency of this process depends on GRB parameters. Estimates are given for the thermal and non-thermal radiation expected to be emitted from the photosphere and the optically thin part of the flow respectively. A critical parameter of the model is the ratio of Poynting flux to kinetic energy flux at some initial radius of the flow. For a large value (100) the non-thermal radiation dominates over the thermal component. If the ratio is small (40) only prompt thermal emission is expected which can be identified with X-ray flashes.
Key words: gamma rays: bursts / magnetic fields / magnetohydrodynamics (MHD) / stars: winds, outflows
© ESO, 2002