On the morphology of supernova remnants with pulsars.

Bhattacharya, D.

Please use this identifier to cite or link to this item: http://hdl.handle.net/2289/734

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DC Field	Value	Language
dc.contributor.author	Bhattacharya, D.	-
dc.date.accessioned	2005-12-16T05:52:25Z	-
dc.date.available	2005-12-16T05:52:25Z	-
dc.date.issued	1990	-
dc.identifier.citation	Journal of Astrophysics and Astronomy, 1990, Vol. 11, p125-140.	en
dc.identifier.issn	0250-6335	-
dc.identifier.uri	http://hdl.handle.net/2289/734	-
dc.description.abstract	One of the intriguing aspects of supernova remnants is their morphology. While the majority of them look like hollow shells, a few, called plerions, are centrally filled like the Crab nebula, and some have a shell-plerion combination morphology. The centrally-filled component in these remnants is believed to be powered by a central pulsar. In this paper results of model calculations of the evolution of surface brightness and morphology of supernova remnants containing pulsars are presented. The paper discusses how the morphology of a supernova remnant will depend on the velocity of expansion, the density of the ambient medium into which it is expanding, and the initial period and magnetic field strength of the central pulsar.	en
dc.format.extent	1656665 bytes	-
dc.format.mimetype	application/pdf	-
dc.language.iso	en	en
dc.publisher	Indian Academy of Sciences, Bangalore, India.	en
dc.rights	Indian Academy of Sciences, Bangalore, India.	en
dc.subject	Remnants;	en
dc.subject	Evolution-Supernova remnants;	en
dc.subject	Morphology-plerions-pulsars;	en
dc.title	On the morphology of supernova remnants with pulsars.	en
dc.type	Article	en
Appears in Collections:	Research Papers (A&A)

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