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Pulsed γ-ray emission from magnetar 1E 2259+586

Published online by Cambridge University Press:  20 March 2013

J. H. K. Wu ,
C. Y. Hui ,
R. H. H. Huang ,
A. K. H. Kong ,
K. S. Cheng ,
J. Takata ,
P. H. T. Tam ,
E. M. H. Wu  and
C.-Y. Liu
J. H. K. Wu
Affiliation:
Institute of Astronomy and Department of Physics, National Tsing Hua University, Hsinchu, Taiwan email: [email protected]
C. Y. Hui
Affiliation:
Department of Astronomy and Space Science, Chungnam National University, Daejeon, Republic of Korea
R. H. H. Huang
Affiliation:
Institute of Astronomy and Department of Physics, National Tsing Hua University, Hsinchu, Taiwan email: [email protected]
A. K. H. Kong
Affiliation:
Institute of Astronomy and Department of Physics, National Tsing Hua University, Hsinchu, Taiwan email: [email protected]
K. S. Cheng
Affiliation:
Department of Physics, University of Hong Kong, Pokfulam Road, Hong Kong
J. Takata
Affiliation:
Department of Physics, University of Hong Kong, Pokfulam Road, Hong Kong
P. H. T. Tam
Affiliation:
Institute of Astronomy and Department of Physics, National Tsing Hua University, Hsinchu, Taiwan email: [email protected]
E. M. H. Wu
Affiliation:
Department of Physics, University of Hong Kong, Pokfulam Road, Hong Kong
C.-Y. Liu
Affiliation:
Institute of Astronomy and Department of Physics, National Tsing Hua University, Hsinchu, Taiwan email: [email protected]
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Abstract

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Anomalous X-ray pulsars (AXPs) are thought to be magnetars which are young isolated neutron stars with extremely strong magnetic fields of >1014 Gauss. Their tremendous magnetic fields inferred from the spin parameters provide a huge energy reservoir to power the observed X-ray emission. High-energy emission above 0.3 MeV has never been detected despite intensive search. Here, we present the possible Fermi Large Area Telescope (LAT) detection of γ-ray pulsations above 200 MeV from the AXP, 1E 2259+586, which puts the current theoretical models of γ-ray emission mechanisms of magnetars into challenge. We speculate that the high-energy γ-rays originate from the outer magnetosphere of the magnetar.

Keywords

gamma rays: observations(stars:) pulsars: individual (1E 2259+586)radiation mechanisms: nonthermal
Type
Contributed Papers
Information
Proceedings of the International Astronomical Union , Volume 8 , Symposium S291: Neutron Stars and Pulsars: Challenges and Opportunities after 80 years , August 2012 , pp. 555 - 557
Copyright
Copyright © International Astronomical Union 2013

References

Abdo, A. A.et al. 2010, ApJ, 725, L73Google Scholar
Castro, D.et al. 2012, arXiv:1207.1432v2Google Scholar
Cheng, K. S. & Zhang, L. 2001, ApJ, 562, 918CrossRefGoogle Scholar
den Hartog, P. R., et al. 2008, A&A, 489, 245Google Scholar
Duncan, R. C. & Thompson, C. 1992, ApJ, 392, L9CrossRefGoogle Scholar
Enoto, T., et al. 2010, Publ. Astron. Soc. Jpn., 62, 475Google Scholar
Icdem, B., Baykal, A. & Inam, S. C. 2012, MNRAS, 419, 3109CrossRefGoogle Scholar
Kuiper, L., Hermsen, W. & Mendez, M. 2004, ApJ, 613, 1173CrossRefGoogle Scholar
Kuiper, L., Hermsen, W., den Hartog, P. R. & Urama, P. R. 2012, ApJ, 748, 133CrossRefGoogle Scholar
Thompson, C. & Duncan, R. C. 1995, MNRAS, 275, 255CrossRefGoogle Scholar
Thompson, C., Lyutikov, M. & Kulkarni, S. R. 2002, ApJ, 574, 332CrossRefGoogle Scholar