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Reverse Shocks in the Relativistic Outflows of Gravitational Wave Detected Neutron Star Binary Mergers

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posted on 2019-09-09, 16:04 authored by Gavin P. Lamb, Shiho Kobayashi
The afterglows to gamma-ray bursts (GRBs) are due to synchrotron emission from shocks generated as an ultra-relativistic outflow decelerates. A forward and a reverse shock will form, however, where emission from the forward shock is well studied as a potential counterpart to gravitational wave-detected neutron star mergers the reverse shock has been neglected. Here, we show how the reverse shock contributes to the afterglow from an off-axis and structured outflow. The off-axis reverse shock will appear as a brightening feature in the rising afterglow at radio frequencies. For bursts at ∼ 100 Mpc, the system should be inclined . 20◦ for the reverse shock to be observable at ∼ 0.1 − 10 days post-merger. For structured outflows, enhancement of the reverse shock emission by a strong magnetic field within the outflow is required for the emission to dominate the afterglow at early times. Early radio photometry of the afterglow could reveal the presence of a strong magnetic field associated with the central engine.

Funding

GPL is supported by STFC grant ST/S000453/1.

History

Citation

Monthly Notices of the Royal Astronomical Society, 489, 1820–1827 (2019)

Author affiliation

/Organisation/COLLEGE OF SCIENCE AND ENGINEERING/Department of Physics and Astronomy

Version

  • VoR (Version of Record)

Published in

Monthly Notices of the Royal Astronomical Society

Volume

489

Pagination

1820-1827

Publisher

Oxford University Press (OUP), Royal Astronomical Society

eissn

1365-2966

Acceptance date

2019-08-11

Copyright date

2019

Available date

2019-08-16

Notes

The file associated with this record is under embargo until publication, in accordance with the publisher's self-archiving policy. The full text may be available through the publisher links provided above.

Language

en

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