Ontology type: schema:ScholarlyArticle
1998-05
AUTHORSC. Kouveliotou, S. Dieters, T. Strohmayer, J. van Paradijs, G. J. Fishman, C. A. Meegan, K. Hurley, J. Kommers, I. Smith, D. Frail, T. Murakami
ABSTRACTSoft |[gamma]|-ray repeaters (SGRs) emit multiple, brief (|[sim]|0.1-s), intense outbursts of low-energy |[gamma]|-rays. They are extremely rare1|[mdash]|three2, 3, 4 are known in our Galaxy and one5 in the Large Magellanic Cloud. Two SGRs are associated5, 6, 7 with young supernova remnants (SNRs), and therefore most probably with neutron stars, but it remains a puzzle why SGRs are so different from |[lsquo]|normal|[rsquo]| radio pulsars. Here we report the discovery of pulsations in the persistent X-ray flux of SGR1806 |[minus]| 20, with a period of 7.47|[thinsp]|s and a spindown rate of 2.6 |[times]| 10|[minus]|3|[thinsp]|s|[thinsp]|yr|[minus]|1. We argue that the spindown is due to magnetic dipole emission and find that the pulsar age and (dipolar) magnetic field strength are |[sim]|1,500 years and 8|[times]| 1014|[thinsp]|gauss, respectively. Our observations demonstrate the existence of |[lsquo]|magnetars|[rsquo]|, neutron stars with magnetic fields about 100 times stronger than those of radio pulsars, and support earlier suggestions8,9 that SGR bursts are caused by neutron-star |[lsquo]|crustquakes|[rsquo]| produced by magnetic stresses. The |[lsquo]|magnetar|[rsquo]| birth rate is about one per millennium|[mdash]|a substantial fraction of that of radio pulsars. Thus our results may explain why some SNRs have no radio pulsars. More... »
PAGES235-237
http://scigraph.springernature.com/pub.10.1038/30410
DOIhttp://dx.doi.org/10.1038/30410
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