Please use this identifier to cite or link to this item:
Full metadata record
DC FieldValueLanguage
dc.contributor.authorKishore, P-
dc.contributor.authorKathiravan, C-
dc.contributor.authorRamesh, R-
dc.contributor.authorEbenezer, E-
dc.identifier.citationJournal of Astrophysics and Astronomy, Vol. 38, No. 2, 24en_US
dc.descriptionOpen Accessen_US
dc.descriptionThe original publication is available at
dc.description.abstractWe recently investigated some of the hitherto unreported observational characteristics of the low frequency (85–35 MHz) type III–V bursts from the Sun using radio spectropolarimeter observations. The quantitative estimates of the velocities of the electron streams associated with the above two types of bursts indicate that they are in the range ≳0.13c≳0.13c –0.02c for the type V bursts, and nearly constant ( ≈0.4c≈0.4c ) for the type III bursts. We also find that the degree of circular polarization of the type V bursts vary gradually with frequency/heliocentric distance as compared to the relatively steeper variation exhibited by the preceding type III bursts. These imply that the longer duration of the type V bursts at any given frequency (as compared to the preceding type III bursts) which is its defining feature, is due to the combined effect of the lower velocities of the electron streams that generate type V bursts, spread in the velocity spectrum, and the curvature of the magnetic field lines along which they travel.en_US
dc.publisherIndian Academy of Sciencesen_US
dc.rights© Indian Academy of Sciences-
dc.subjectMagnetic fielden_US
dc.subjectRadio burstsen_US
dc.titleCoronal magnetic field lines and electrons associated with type III–V radio bursts in a solar flareen_US
Appears in Collections:IIAP Publications

Files in This Item:
File Description SizeFormat 
Coronal Magnetic Field Lines and Electrons Associated with.pdfOpen Access 2.12 MBAdobe PDFView/Open

Items in DSpace are protected by copyright, with all rights reserved, unless otherwise indicated.