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Radio evidence for shock acceleration of electrons in the solar corona
Author(s) -
Cane H. V.,
Stone R. G.,
Fainberg J.,
Stewart R. T.,
Steinberg J. L.,
Hoang S.
Publication year - 1981
Publication title -
geophysical research letters
Language(s) - English
Resource type - Journals
SCImago Journal Rank - 2.007
H-Index - 273
eISSN - 1944-8007
pISSN - 0094-8276
DOI - 10.1029/gl008i012p01285
Subject(s) - physics , astrophysics , wavelength , shock (circulatory) , astronomy , shock wave , acceleration , electron , radio wave , observatory , solar radio , particle acceleration , corona (planetary geology) , optics , astrobiology , medicine , classical mechanics , venus , quantum mechanics , thermodynamics
A new class of kilometer wavelength solar radio bursts has been observed with the ISEE‐3 Radio Astronomy Experiment. These events resemble groups of ordinary type III bursts but have some unique properties. They are very intense and have durations considerably longer than groups of type III bursts. The new class of events do not necessarily occur at the times of reported meter wavelength type III activity and therefore do not appear to be the continuation of such activity to long wavelengths. Instead they occur at the reported times of type II events, which are indicative of a shock wave. An examination of records from the Culgoora Radio Observatory shows that the associated type II bursts have fast drift elements emanating from them i.e. herringbone structure. It is proposed that the new class of bursts are the long wavelength continuation of herringbone structure and it seems probable that the electrons producing the radio emission are accelerated by shocks. The new type of events will be referred to as shock accelerated (SA) events. The characteristics of SA events are discussed.