Nova Persei 1901 (GK Per): A miniature supernova remnant

Details Nova Persei 1901 (GK Per): A miniature supernova remnant Nova Persei 1901 (GK Per): A miniature supernova remnant

Jan 2002

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2002aspc..261..617b&link_type=abstract

The Physics of Cataclysmic Variables and Related Objects, ASP Conference Proceedings, Vol. 261. Edited by B. T. Gänsicke, K. Beu

Physics

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Scientific paper

I present the Chandra ACIS-S data of the shell of the classical Nova Persei (1901). The X-ray nebula is detected with a count rate of 0.0925 +/-0.01 c s-1. It is lumpy and asymmetric with the bulk of emission on the southwestern quadrant. The X-ray emission from the vicinity of the radio ridge is detected as an arc that covers from west to south of the central source. The X-ray nebula is affected mostly by the complex interstellar medium around the nova and thus have not developed a regular shell. The X-ray spectrum consists at least of two thermal components of emission. The maximum mass in the X-ray emitting nebula is estimated as 5 times 10-4 Modot. The X-ray luminosities ~1031 erg s-1 indicate that the shock is adiabatic and the remnant is most likely in an early phase of evolution (Pre-Sedov/Transition to Sedov).

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