On the approach to stability of pulsar average profiles

Rathnasree, N.; Rankin, J.M.

Please use this identifier to cite or link to this item: http://hdl.handle.net/2289/1401

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DC Field	Value	Language
dc.contributor.author	Rathnasree, N.	-
dc.contributor.author	Rankin, J.M.	-
dc.date.accessioned	2006-07-07T06:05:30Z	-
dc.date.available	2006-07-07T06:05:30Z	-
dc.date.issued	1995-10	-
dc.identifier.citation	Astrophysical Journal, 1995, Vol.452, p814-818	en
dc.identifier.issn	0004-637X	-
dc.identifier.issn	1538-4357 (online)	-
dc.identifier.uri	http://hdl.handle.net/2289/1401	-
dc.description.abstract	We have studied the rate of stabilization to a global average profile for over two dozen radio pulsars. To investigate the physical processes governing the approach to a stable profile, the pulse-to-pulse profile variations have been separated into three components: variations arising from the changes in the intensity, phase, and width of the pulse maximum. The rate of stabilization is seen to vary from pulsar to pulsar, and a correlation analysis of this rate with other pulsar properties gives some insight into the processes governing irregular variations from pulse to pulse. The stabilization rate for the polarized emission has also been studied, and it is seen that this rate generally is slower than the stabilization rate for the total intensity. In many cases there is a sharp change in the stabilization rate after approximately 4-100 pulses are averaged.	en
dc.format.extent	734724 bytes	-
dc.format.mimetype	application/pdf	-
dc.language.iso	en	en
dc.publisher	The University of Chicago Press for the American Astronomical Society	en
dc.relation.uri	http://adsabs.harvard.edu/cgi-bin/bib_query?1995ApJ...452..814R	en
dc.rights	(1995) by the American Astronomical Society. Scanned images provided by the NASA ADS Data System.	en
dc.subject	Stars	en
dc.subject	Pulsars	en
dc.title	On the approach to stability of pulsar average profiles	en
dc.type	Article	en
Appears in Collections:	Research Papers (A&A)

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