Radio emission as a diagnostic for solar coronal rotation

dc.contributor.author	Vats, H. O
dc.contributor.author	Deshpande, M. R
dc.contributor.author	Mehta, M
dc.contributor.author	Shah, C. R
dc.contributor.author	Shah, K. J
dc.date.accessioned	2007-10-16T09:27:26Z
dc.date.available	2007-10-16T09:27:26Z
dc.date.issued	1999
dc.identifier.citation	BASI, Vol. 27, No. 1, pp. 61 - 63	en
dc.identifier.uri	http://hdl.handle.net/2248/1888
dc.description.abstract	The time series of solar radio emission at 2.8 GHz is analysed using correlation methods. The analysis showed that this type of time series can be used to infer the rotation period of the source (in this case solar corona). It is found that the correlograms have a very strong persistence of rotational modulation. These values are significantly lower than those reported earlier by other methods. The reasons for this difference are unknown.	en
dc.format.extent	256748 bytes
dc.format.mimetype	application/pdf
dc.language.iso	en	en
dc.publisher	Astronomical Society of India	en
dc.relation.uri	http://adsabs.harvard.edu/abs/1999BASI...27...61V	en
dc.subject	Radio emission	en
dc.subject	Solar radio emission	en
dc.subject	Coronal rotation	en
dc.title	Radio emission as a diagnostic for solar coronal rotation	en
dc.type	Article	en