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X-Ray Emission Differences in SNR MSH14-63

Published online by Cambridge University Press:  14 August 2015

Fangjun Lu ,
Mei Wu ,
Tipei Li  and
Xuejun Sun
Fangjun Lu
Affiliation:
High Energy Astrophysics Lab, Institute of High Energy Physics, Academia Sinica, Beijing 100039, P.R. China
Mei Wu
Affiliation:
High Energy Astrophysics Lab, Institute of High Energy Physics, Academia Sinica, Beijing 100039, P.R. China
Tipei Li
Affiliation:
High Energy Astrophysics Lab, Institute of High Energy Physics, Academia Sinica, Beijing 100039, P.R. China
Xuejun Sun
Affiliation:
High Energy Astrophysics Lab, Institute of High Energy Physics, Academia Sinica, Beijing 100039, P.R. China and Beijing Astronomical Observatory, Academia Sinica, Beijing 100080, P.R. China

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In the paper we report the discovery of X-ray emission differences in SNR MSH14-63 based on the ROSAT PSPC observation. The structures of MSH14-63 are different in different energy bands. These images along with the radial brightness distributions in these energy bands show the existence of a region which only emit X-ray photons harder than l.OkeV. Though weak, there actually exist large scale X-ray emissions beyond the bright rim in many parts of the northeast remnant component, which is in conflict with the Sedov phase assumption used in previous research. These new soft X-ray features provide astronomers more information to study its physical characteristics.

Type
II. Joint Discussions
Information
Highlights of Astronomy , Volume 11 , Issue 1: Highlights of Astronomy. As presented at the XXIIIrd General Assembly of the IAU (Part A), 1997 , 1998 , pp. 393
Copyright
Copyright © Kluwer 1998