Magnetars: Soft Gamma Repeaters

Details Magnetars: Soft Gamma Repeaters Magnetars: Soft Gamma Repeaters

Jul 2004

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2004aipc..714..273k&link_type=abstract

X-RAY TIMING 2003: Rossie and Beyond. AIP Conference Proceedings, Volume 714, pp. 273-280 (2004).

Physics

Neutron Stars, X-Ray, Gamma-Ray

Scientific paper

Magnetars are a subclass of highly magnetized neutron stars characterized by their recurrent X-ray bursts. While in an active (bursting) state, they are emitting hundreds of predominantly soft (kT = 30 keV), and short (0.1 - 100 ms long) events. Active states last anywhere between days and years. The magnetar quiescent source X-ray light curves exhibit pulsations in the narrow range of 5 - 11 s; estimates of their spin-down rates indicate that their magnetic fields are extremely high, of the order of 1014 - 1015 G. Such high B-field objects, had been predicted to exist in 1992, and were confirmed observationally with RXTE in 1998. Two types of sources are magnetar candidates to date: Soft Gamma Repeaters and Anomalous X-ray Pulsars. This review is focused on the history of Soft Gamma Repeaters and their spectral, timing and flux characteristics, both in their persistent and their burst emission.

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