Estimation of coronal magnetic fields using Type-I emission

dc.contributor.author	Gopalswamy, N
dc.contributor.author	Thejappa, G
dc.contributor.author	Sastry, Ch. V
dc.contributor.author	Tlamicha, A
dc.date.accessioned	2009-01-07T12:27:09Z
dc.date.available	2009-01-07T12:27:09Z
dc.date.issued	1986-03
dc.identifier.citation	Bulletin of Astronomical Institutes of Czechoslovakia, Vol. 37, pp. 115 - 120	en
dc.identifier.issn	0004-6248
dc.identifier.uri	http://hdl.handle.net/2248/4243
dc.description.abstract	The radial dependence of the coronal magnetic field above active regions is calculated using Type-I chain data existing in the literature. Assuming that Type-I emission is due to shock waves, the upstream shock velocity and the density jump across the shock are obtained respectively from the drift rate and the bandwidth of the Type-I chains. Making use of the shock velocity and the density jump in the Rankine-Hugoniot relation, the Alfvén velocity and hence the magnetic field in the corona is calculated. The results are compared with existing estimates.	en
dc.language.iso	en	en
dc.publisher	Czechoslovakia Academy of Sciences	en
dc.relation.uri	http://adsabs.harvard.edu/abs/1986BAICz..37..115G	en
dc.subject	Coronal Loops	en
dc.subject	Solar Corona	en
dc.subject	Solar Magnetic Field	en
dc.subject	Solar Radio Bursts	en
dc.subject	Propagation Velocity	en
dc.subject	Rankine-Hugoniot Relation	en
dc.subject	Shock Wave Propagation	en
dc.subject	Solar Activity	en
dc.title	Estimation of coronal magnetic fields using Type-I emission	en
dc.type	Article	en