A detailed X-ray investigation of PSR J2021+4026 and the γ-Cygni supernova remnant

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題名:	A detailed X-ray investigation of PSR J2021+4026 and the γ-Cygni supernova remnant
作者:	周翊;Hui, C. Y.;Seo, K. A.;Lin, L. C. C.;Huang, R. H. H.;Hu, C. P.;Wu, J. H. K.;Trepl, L.;Takata, J.;Wang, Y.;Chou, Y.;Cheng, K. S.;Kong, A. K. H.
貢獻者:	理學院天文研究所
關鍵詞:	ASTROPHYSICS, COSMOLOGY AND ASTRONOMY;COMPARATIVE EVALUATIONS;Emission;Extrapolation;IONIZATION;NEBULAE;NEUTRON STARS;NEUTRONS;Orientation;PHOTONS;PROPER MOTION;PULSARS;PULSATIONS;SHOCK WAVES;STELLAR WINDS;SUPERNOVA REMNANTS;SUPERNOVAE;X RADIATION;X-rays;XMM (spacecraft)
日期:	2015-01-20
上傳時間:	2026-04-21 14:31:56 (UTC+8)
出版者:	IOP Publishing Ltd.;United States
摘要:	摘要： We have investigated the field around the radio-quiet gamma -ray pulsar, PSR J2021+4026, with a ~140 ks XMM-Newton observation and ~56 ks archival Chandra data. In re-analyzing the Chandra data, we have confirmed the presence of a bow-shock nebula that extends from the pulsar to the west by ~10 arcsec. The orientation of this nebular feature suggests that the pulsar is probably moving eastward, which is consistent with the speculated proper motion by extrapolating from the nominal geometrical center of the supernova remnant (SNR) G78.2+2.1 to the current pulsar position. The remnant emission in both of the examined regions is in a non-equilibrium ionization state. Also, the elapsed time of both regions after shock-heating is apparently shorter than the Sedov age of G78.2+2.1. This might suggest that the reverse shock has reached the center not long ago. Apart from PSR J2021+4026 and G78.2+2.1, we have also serendipitously detected an X-ray flash-like event, XMM J202154.7+402855, from this XMM-Newton observation. 出版者： United States 出版日期： 2015-01-20 出處： The Astrophysical journal, 2015-01, Vol.799 (1), p.76-15 資源來源： Institute of Physics Journals 識別號： ISSN: 1538-4357 識別號： ISSN: 0004-637X 識別號： EISSN: 1538-4357 識別號： DOI: 10.1088/0004-637X/799/1/76
顯示於類別:	[天文研究所] 期刊論文

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