The large scale structure of the Galactic magnetic field

Indrani, C.; Deshpande, A.A.

Please use this identifier to cite or link to this item: http://hdl.handle.net/2289/5356

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DC Field	Value	Language
dc.contributor.author	Indrani, C.	-
dc.contributor.author	Deshpande, A.A.	-
dc.date.accessioned	2007-01-08T09:14:52Z	-
dc.date.available	2007-01-08T09:14:52Z	-
dc.date.issued	1998	-
dc.identifier.citation	New Astronomy, 1998, Vol.4, p33	en
dc.identifier.issn	1384-1076	-
dc.identifier.uri	http://hdl.handle.net/2289/5356	-
dc.description	Restricted Access.	en
dc.description.abstract	We explore the possibility of refining the description for the large-scale magnetic field in our galaxy using the rotation measures (RM) of pulsars. A major new input in our analysis is the recent comprehensive model of the electron density distribution (Taylor & Cordes, 1993) that explicitly accounts for the electron density variations due to the spiral structure in our galaxy. We examine various models to assess the possibility that the magnetic field strength and the electron density may have correlated variations. Our analysis shows that in most of the regions the `net' field is stronger in the interarm regions rather than in the spiral arms, and the model in which the large-scale magnetic field is positively correlated with the electron density can be rejected with a high degree of confidence based on the pulsar RM data. (C) 1998 Elsevier Science B. V. All rights reserved.	en
dc.language.iso	en	en
dc.publisher	Elsevier B. V.	en
dc.rights	1998 Elsevier B.V.	en
dc.subject	ISM	en
dc.subject	Magnetic fields	en
dc.subject	Galaxies	en
dc.subject	Pulsars	en
dc.title	The large scale structure of the Galactic magnetic field	en
dc.type	Article	en
Appears in Collections:	Research Papers (A&A)

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