Characteristics of coronal shock waves and solar type II radio bursts.

Details Characteristics of coronal shock waves and solar type II radio bursts. Characteristics of coronal shock waves and solar type II radio bursts.

Mar 1995

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1995a%26a...295..775m&link_type=abstract

Astronomy and Astrophysics, v.295, p.775

Astronomy and Astrophysics

Astrophysics

49

Sun: Corona: Radio Radiation, Plasmas, Shock Waves

Scientific paper

In the solar corona shock waves can be generated by coronal mass ejections and solar flares. They manifest themselves in solar type II radio bursts. These special bursts appear as narrow emission stripes drifting slowly from high to low frequencies in dynamic radio spectra. A sample of 25 solar type II radio bursts observed in the range of 40-170MHz by the radio spectrograph of the Astrophysikalisches Institut Potsdam is investigated concerning their spectral features, i.e., drift rate and instantaneous bandwidth. Plasma waves measurements at interplanetary shock waves provide the assumption that type II radio emission is originated in the vicinity of the transition region of shock waves. Thus, the instantaneous bandwidth of a solar type II radio burst would reflect the density jump across the associated shock wave. In the framework of magnetohydrodynamics the Rankine- Hugoniot relations of shock waves are investigated under circumstances of the upper corona. Comparing these results with those obtained from the observational study solar type II radio bursts should be considered to be generated either by weak supercritical, quasi-parallel, or by subcritical, quasi- perpendicular fast magnetosonic shock waves in the corona.

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