Physics
Scientific paper
Apr 1990
adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1990ipesprept.....b&link_type=abstract
M.S. Thesis - 5 Jun. 1989 Instituto de Pesquisas Espaciais, Sao Jose dos Campos (Brazil).
Physics
Chromosphere, Coronas, Plasmas (Physics), Radio Emission, Radio Observation, Solar Activity, Type 3 Bursts, X Rays, Ambiguity, Electrons, Remote Sensing, Solar Maximum Mission, Temporal Resolution
Scientific paper
In all previous attempts to show one-to-one correlation between type 3 bursts and x ray spikes, there have always been ambiguities as to which of several x ray spikes are correlated with any given type 3 burst. Observations are presented that show clear associations of x ray bursts with RS type 3 bursts between 16:46 UT and 16:52 UT on 1985, July 9. The hard x ray observations were made at energies above 25 keV with HXRBS on SMM and the radio observations were made at 1.63 GHz using the 13.7 m diameter in Itapetinga antenna in R and L polarization with a time resolution of 3 ms. Detailed comparison between the hard x ray and radio observations shows: (1) That in at least 12 cases the associated hard x ray and decimetric RS bursts can be identified; and (2) on the average, the x ray peaks were delayed from the peak of the RS bursts at 1.6 GHz by approximately 400 ms although a delay as long as 1 sec was observed in one case. One possible explanation of the long delays between the RS bursts and the associated x ray bursts is that the RS burst is produced at the leading edge of the electron beam whereas the x ray burst peaks at the time of arrival of the bulk of the electrons at the high density region mostly at the lower corona and upper chromosphere. Thus, comparison must be made between the time the peak of the radio pulse and the start of the x ray burst. In that case the delays are consistent with an electron travel time of approximately 0.3 c from the 800 MHz plasma level to the lower corona assuming that the radio emission is at the second harmonic.
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