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Central compact objects and their magnetic fields

Published online by Cambridge University Press:  20 March 2013

Wynn C. G. Ho
Wynn C. G. Ho*
Affiliation:
School of Mathematics, University of Southampton, Southampton, SO17 1BJ, UK email: [email protected]
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Abstract

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Central compact objects (CCOs) are neutron stars that are found near the center of supernova remnants, and their association with supernova remnants indicates these neutron stars are young (≲ 104 yr). Here we review the observational properties of CCOs and discuss implications, especially their inferred magnetic fields. X-ray timing and spectral measurements suggest CCOs have relatively weak surface magnetic fields (~ 1010 − 1011 G). We argue that, rather than being created with intrinsically weak fields, CCOs are born with strong fields and we are only seeing a weak surface field that is transitory and evolving. This could imply that CCOs are one manifestation in a unified picture of neutron stars.

Keywords

pulsars: generalstars: magnetic fieldstars: neutronsupernova remnants
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. 101 - 106
Copyright
Copyright © International Astronomical Union 2013

References

Becker, W., Prinz, T., Winkler, P. F., & Petre, R. 2012, ApJ, 755, 141Google Scholar
Bernal, C. G., Lee, W. H., & Page, D. 2010, Revista Mexicana de Astron. Astrof., 46, 301Google Scholar
Bignami, G. F., Caraveo, P. A., Luca, A. D., & Mereghetti, S. 2003, Nature, 423, 725Google Scholar
Chevalier, R. A. 1989, ApJ, 346, 847Google Scholar
De Luca, A. 2008, in: Bassa, C. G.et al. (eds.), AIP Conf. Proc. Vol. 983, 40 Years of Pulsars (Melville: American Inst. Phys.), p. 311Google Scholar
De Luca, A.et al. 2004, A&A, 418, 625Google Scholar
De Luca, A.et al. 2011, A&A, 525, A106Google Scholar
De Luca, A.et al. 2012, MNRAS, 421, L72CrossRefGoogle Scholar
Faucher-Giguère, C.-A. & Kaspi, V. M. 2006, ApJ, 643, 332Google Scholar
Geppert, U., Page, D., & Zannias, T. 1999, A&A, 345, 847Google Scholar
Goldreich, P. & Reisenegger, A. 1992, ApJ, 395, 250Google Scholar
Gotthelf, E. V. & Halpern, J. P. 2008, in: Bassa, C. G.et al. (eds.), AIP Conf. Proc. Vol. 983, 40 Years of Pulsars (Melville: American Inst. Phys.), p. 320Google Scholar
Gotthelf, E. V. & Halpern, J. P. 2009, ApJ, 695, L35Google Scholar
Gotthelf, E. V., Perna, R., & Halpern, J. P. 2010, ApJ, 724, 1316Google Scholar
Halpern, J. P. & Gotthelf, E. V. 2010, ApJ, 709, 436CrossRefGoogle Scholar
Halpern, J. P. & Gotthelf, E. V. 2011, ApJ, 733, L28Google Scholar
Halpern, J. P., Gotthelf, E. V., Camilo, F., & Seward, F. D. 2007, ApJ, 665, 1304Google Scholar
Ho, W. C. G. 2007, MNRAS, 380, 71Google Scholar
Ho, W. C. G. 2011, MNRAS, 414, 2567Google Scholar
Ho, W. C. G. 2012, MNRAS, submitted (arXiv:1208.1297)Google Scholar
Ho, W. C. G. & Andersson, N. 2012, Nature Physics, in press (arXiv:1208.3201)Google Scholar
Ho, W. C. G. & Heinke, C. O. 2009, Nature, 462, 71Google Scholar
Ho, W. C. G. & Lai, D. 2001, MNRAS, 327, 1081CrossRefGoogle Scholar
Ho, W. C. G. & Mori, K. 2008, in: Bassa, C. G.et al. (eds.), AIP Conf. Proc. Vol. 983, 40 Years of Pulsars (Melville: American Inst. Phys.), p. 340Google Scholar
Ho, W. C. G., Potekhin, A. Y., & Chabrier, G. 2008, ApJS, 178, 102Google Scholar
Kaspi, V. M. 2010, Proc. National Academy Sci., 16, 7147Google Scholar
Lai, D. 2001, Rev. Mod. Phys., 73, 629Google Scholar
Manchester, R. N., Hobbs, G. B., Teoh, A., & Hobbs, M. 2005, AJ, 129, 1993Google Scholar
Muslimov, A. & Page, D. 1995, ApJ, 440, L77Google Scholar
Muslimov, A. & Page, D. 1996, ApJ, 458, 347Google Scholar
Pavlov, G. G. & Panov, A. N. 1976, Sov. Phys. JETP, 44, 300Google Scholar
Pavlov, G. G., Shibanov, Yu. A., & Yakovlev, D. G. 1980, Ap&SS, 73, 33Google Scholar
Pons, J. A., Viganò, D., & Geppert, U. 2012, A&A, 547, A9Google Scholar
Popov, S. B., et al. 2010, MNRAS, 401, 2675CrossRefGoogle Scholar
Potekhin, A. Y. 2010, A&A, 518, A24Google Scholar
Potekhin, A. Y. & Chabrier, G. 2003, ApJ, 585, 955CrossRefGoogle Scholar
Roger, R. S., et al. 1988, ApJ, 332, 940Google Scholar
Romani, R. W. 1990, Nature, 347, 741Google Scholar
Sanwal, D., Pavlov, G. G., Zavlin, V. E., & Teter, M. A. 2002, ApJ, 574, L61Google Scholar
Shabaltas, N. & Lai, D. 2012, ApJ, 748, 148Google Scholar
Spitkovsky, A. 2006, ApJ, 648, L51Google Scholar
Suleimanov, V. F., Pavlov, G. G., & Werner, K. 2010, ApJ, 714, 630Google Scholar
Suleimanov, V. F., Pavlov, G. G., & Werner, K. 2012, ApJ, 751, 15Google Scholar
Sun, M., Seward, F. D., Smith, R. K., & Slane, P. O. 2004, ApJ, 605, 742Google Scholar
Viganò, D. & Pons, J. A. 2012, MNRAS, 425, 2487Google Scholar
Zavlin, V. E. 2009, in: Becker, W. (ed.), Ap&SS Lib. Vol. 357, Neutron Stars and Pulsars (Berlin: Springer-Verlag), p. 181Google Scholar