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Year-scale Morphological Variation of the X-ray Crab Nebula

Published online by Cambridge University Press:  19 July 2016

Koji Mori ,
David N. Burrows ,
George G. Pavlov ,
J. Jeff Hester ,
Shinpei Shibata  and
Hiroshi Tsunemi
Koji Mori
Affiliation:
Department of Astronomy and Astrophysics, 525 Davey Laboratory, The Pennsylvania State University, University Park, PA 16802, USA
David N. Burrows
Affiliation:
Department of Astronomy and Astrophysics, 525 Davey Laboratory, The Pennsylvania State University, University Park, PA 16802, USA
George G. Pavlov
Affiliation:
Department of Astronomy and Astrophysics, 525 Davey Laboratory, The Pennsylvania State University, University Park, PA 16802, USA
J. Jeff Hester
Affiliation:
Department of Physics and Astronomy, Arizona State University, Tempe, AZ 85287-1504, USA
Shinpei Shibata
Affiliation:
Department of Physics, Yamagata University, Yamagata 990-8560, Japan
Hiroshi Tsunemi
Affiliation:
Department of Earth and Space Science, Graduate School of Science, Osaka University, 1-1 Machikaneyama, Toyonaka, Osaka 560-0043, Japan

Abstract

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We present year-scale morphological variations of the Crab Nebula revealed by the Chandra X-ray Observatory. Observations have been performed about every 1.7 years over the three years from launch. The variations are clearly recognized at two sites: the torus and the southern jet. The torus, which had been steadily expanding until 1.7 years ago, now appears to have shrunk in the latest observation. Additionally, the circular structures seen to the northeast of the torus have decayed into several arcs. On the other hand, the southern jet shows the growth of its overall kinked-structure. We discuss the nature of these variations in terms of the pulsar wind nebula mechanism.

Type
Part 4: Pulsar Wind Nebulae and Their Environments
Information
Symposium - International Astronomical Union , Volume 218: Young Neutrons Stars and their Environments , 2004 , pp. 181 - 184
Copyright
Copyright © Astronomical Society of the Pacific 2004 

References

Begelman, M. C. 1998, ApJ, 493, 291.CrossRefGoogle Scholar
Greiveldinger, C., & Aschenbach, B. 1999, ApJ, 510, 305.Google Scholar
Hester, J. J. et al. 2002, ApJ, 577, 871.Google Scholar
Kennel, C. F., & Coroniti, F. V. 1984, ApJ, 283, 694.Google Scholar
Mori, K. et al. 2002, in ASP Conf. Series, Vol. 271, Neutron Stars in Supernova Remnants, eds. Slane, P. O., & Gaensler, B. M., (San Francisco: ASP), p. 157.Google Scholar
Mori, K. 2002, PhD thesis, Osaka University.Google Scholar
Pavlov, G. G. et al. 2003, ApJ, 591, 1157.Google Scholar
Weisskopf, M. et al. 2000, ApJ, 536, 81.Google Scholar