An X-ray pulsar with a superstrong magnetic field in the soft γ-ray repeater SGR1806 − 20

C. Kouveliotou (), S. Dieters, T. Strohmayer, J. van Paradijs, G. J. Fishman, C. A. Meegan, K. Hurley, J. Kommers, I. Smith, D. Frail and T. Murakami
Additional contact information
C. Kouveliotou: ES-84, Space Science Laboratory, NASA/Marshall Space Flight Center
S. Dieters: ES-84, Space Science Laboratory, NASA/Marshall Space Flight Center
T. Strohmayer: Universities Space Research Association
J. van Paradijs: University of Alabama in Huntsville
G. J. Fishman: ES-84, Space Science Laboratory, NASA/Marshall Space Flight Center
C. A. Meegan: ES-84, Space Science Laboratory, NASA/Marshall Space Flight Center
K. Hurley: Space Sciences Laboratory, University of California
J. Kommers: Massachusetts Institute of Technology
I. Smith: Rice University, Space Physics and Astronomy
D. Frail: NRAO, VLA
T. Murakami: ISAS

Nature, 1998, vol. 393, issue 6682, 235-237

Abstract: Abstract Soft γ-ray repeaters (SGRs) emit multiple, brief (∼0.1-s), intense outbursts of low-energy γ-rays. They are extremely rare1—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 ‘normal’ radio pulsars. Here we report the discovery of pulsations in the persistent X-ray flux of SGR1806 − 20, with a period of 7.47 s and a spindown rate of 2.6 × 10−3 s yr−1. We argue that the spindown is due to magnetic dipole emission and find that the pulsar age and (dipolar) magnetic field strength are ∼1,500 years and 8× 1014 gauss, respectively. Our observations demonstrate the existence of ‘magnetars’, 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 ‘crustquakes’ produced by magnetic stresses. The ‘magnetar’ birth rate is about one per millennium—a substantial fraction of that of radio pulsars. Thus our results may explain why some SNRs have no radio pulsars.

Date: 1998
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DOI: 10.1038/30410

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