Please use this identifier to cite or link to this item: http://hdl.handle.net/2248/198
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dc.contributor.authorThejappa, G-
dc.date.accessioned2005-01-08T06:41:23Z-
dc.date.available2005-01-08T06:41:23Z-
dc.date.issued1988-
dc.identifier.citationKodaikanal Observatory Bulletins Series A, Vol. 9, pp. 165-176en
dc.identifier.issn0374-3632-
dc.identifier.urihttp://hdl.handle.net/2248/198-
dc.description.abstractThe slowly drifting solar type II radio bursts are believed to be due to the flare associated shock waves propagating radially outward in the corona. The main observational characteristics of these bursts show that the shocks responsible are supercritical and quasiperpendicular. The electrons accelerated through reflected-ion-beam-excited low frequency waves form gap distributions by getting scattered on whistlers and they fill a large volume just in front and behind the shock front rise to the backbone emission. The electrons accelerated by fast Fermi process form electron beam escaping from the shock front and give rise to herringbone emission. The brightness temperatures, polarization and frequency splitting are self consistently explained.en
dc.format.extent399027 bytes-
dc.format.mimetypeapplication/pdf-
dc.language.isoen-
dc.publisherIndian Institute of Astrophysics, Bangaloreen
dc.subjectRadio emissionen
dc.subjectSolar Coronaen
dc.subjectCoronal type II bursten
dc.titleRadio emission from the Solar Corona due to shock wavesen
dc.typeArticleen
Appears in Collections:IIAP Publications
Kodaikanal Observatory Bulletins (1905 - 1997 )

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