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Infrared AKARI observations of magnetars 4U 0142+61 and 1E 2259+586

Published online by Cambridge University Press:  20 March 2013

Takayoshi Kohmura ,
Kenta Kaneko ,
Shoma Ikeda ,
Mikio Morii ,
Katsuaki Asano ,
Mai Shirahara  and
Noriaki Shibazaki
Takayoshi Kohmura
Affiliation:
Physics Department, Kogakuin University, 2665-1, Nakano-cho, Hachioji, Tokyo, 192-0015, Japan email: tkohmura@map.kogakuin.ac.jp
Kenta Kaneko
Affiliation:
Physics Department, Kogakuin University, 2665-1, Nakano-cho, Hachioji, Tokyo, 192-0015, Japan email: tkohmura@map.kogakuin.ac.jp
Shoma Ikeda
Affiliation:
Physics Department, Kogakuin University, 2665-1, Nakano-cho, Hachioji, Tokyo, 192-0015, Japan email: tkohmura@map.kogakuin.ac.jp
Mikio Morii
Affiliation:
Department of Physics, Tokyo Institute of Technology, 2-12-1, Ookayama, Meguro-ku, Tokyo, 152-8551, Japan
Katsuaki Asano
Affiliation:
Department of Physics, Tokyo Institute of Technology, 2-12-1, Ookayama, Meguro-ku, Tokyo, 152-8551, Japan
Mai Shirahara
Affiliation:
Institute of Space and Astronautical Science, JAXA, 3-1-1 Yoshinodai, Sagamihara, Kanagawa, 229-8510, Japan
Noriaki Shibazaki
Affiliation:
Department of Physics, Rikkyo University, 3-34-1, Nishi-ikebukuro, Toshima-ku, Tokyo, 171-8501, Japan
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Abstract

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We observed two magnetars, 4U 0142+61 and 1E2259+568, with the Japanese infrared satellite AKARI to search for the time variability at wavelengths between 2-4 μm. We significantly detected 4U0142+61 in the 4μm band, and determined flux upper limits in the other two bands. We did not detect 1E 2259+586 in any of the bands, and determined upper limits. Comparing the detection of 4U 0142+61 in the 4μm band with the Spitzer observation from 2005, we found the flux was reduced to be 64%. We interpret this time variability in the infrared band as an increase of the inner radius of the dust disk around the neutron star, where the increase is due to the sublimation of the dust by the large flare of neutron star itself.

Keywords

stars: neutron – infrared: stars – X-rays: individual (4U 0142+61, 1E 2259+586)
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. 422 - 424
Copyright
Copyright © International Astronomical Union 2013

References

Kaplan, D. L., et al. 2009, ApJ, 700, 149CrossRefGoogle Scholar
Wang, Z., et al. 2006, Nature, 440, 772CrossRefGoogle Scholar
Kaneko, K., Kohmura, T., et al. 2012, in prep.Google Scholar
Kohmura, T., Kaneko, K., et al. 2012, in prep.Google Scholar
Vertilek, S. D., et al. 1990, A&A 235 162–173Google Scholar