Astronomy and Astrophysics – Astrophysics – High Energy Astrophysical Phenomena
Scientific paper
2011-09-24
MNRAS, 421, 2442-2466 (2012)
Astronomy and Astrophysics
Astrophysics
High Energy Astrophysical Phenomena
53 pages, 10 figures, accepted to MNRAS (the abstract and introduction are now easier to follow)
Scientific paper
10.1111/j.1365-2966.2012.20473.x
Important astrophysical sources, such as gamma-ray bursts (GRBs) or tidal disruption events, are impulsive -- strongly varying with time. These outflows are likely highly magnetized near the central source, but their interaction with the external medium is not yet fully understood. Here I consider the combined impulsive magnetic acceleration of an initially highly magnetized shell of plasma and its deceleration by the external medium. I find four main dynamical regimes, that (for a given outflow) depend on the external density. (I) For small enough external densities the shell becomes kinetically dominated before it is significantly decelerated, thus reverting to the familiar unmagnetized "thin shell" case, which produces bright reverse shock emission that peaks well after the prompt GRB. (II) For larger external densities the shell remains highly magnetized and the reverse shock is strongly suppressed. It eventually transfers most of its energy through pdV work to the shocked external medium, whose afterglow emission peaks on a timescale similar to the prompt GRB duration. (III) For even larger external densities there is no initial impulsive acceleration phase. (IV) For the highest external densities the flow remains Newtonian.
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