Radio emission from solar and stellar coronae

Details Radio emission from solar and stellar coronae Radio emission from solar and stellar coronae

Mar 1982

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1982phdt.........5g&link_type=abstract

Ph.D. Thesis Colorado Univ., Boulder.

Physics

7

Radio Emission, Radio Physics, Solar Radio Bursts, Stellar Coronas, Coronagraphs, Density Measurement, Plasma Radiation, Polarimeters

Scientific paper

Several problems in radiophysics are explored. Polarization measurements f two types of solar bursts--Reverse Drift Pairs and Type V bursts--allowed identification of the radiation as due to fundamental plasma emission for RDPs and harmonic plasma emission for Type Vs. Two other types of solar radio burst--Type II (shock related) and Type IV are studied with the aid of coronagraph/polarimeter (C/P) observations. Together, the radio and C/P data indicate the presence of two separate shocks in the coronal transient event. One shock, without radio emission, led the transient and was driven by it. Estimates of the density enhancement caused by the shock give Mach number 1.2 MA 3 and, hence, magnetic field strength in the ambient corona 0.05 B gauss. The second shock, which gave rise to the radio emission, was associated with the loops.

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