Coronal evolution and solar type I radio bursts - an ion-acoustic wave model

Details Coronal evolution and solar type I radio bursts - an ion-acoustic wave model Coronal evolution and solar type I radio bursts - an ion-acoustic wave model

Jan 1981

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1981a%26a....94..100b&link_type=abstract

Astronomy and Astrophysics, vol. 94, no. 1, Jan. 1981, p. 100-108. Research supported by the Eidgenoessische Technische Hochsch

Astronomy and Astrophysics

Astrophysics

63

Ion Acoustic Waves, Noise Storms, Solar Corona, Solar Radio Bursts, Solar Storms, Brightness Temperature, Magnetohydrodynamic Waves, Plasma Waves, Solar Flux Density, Sunspots, Trapped Particles, Type 3 Bursts, Wave Interaction

Scientific paper

A model is proposed for type I burst emission that can accommodate both the main burst observations and an origin for the continuum. It is assumed that ion-acoustic waves are generated in the burst source by a current that is related to the coronal magnetic evolution, in particular to magnetic nonequilibrium caused by photospheric changes (e.g. emerging magnetic field) in active regions. Radio emission arises from coalescence of ion-acoustic and plasma waves. Contrary to other plasma wave models, emission at the harmonic of the plasma frequency is below the present detection threshold (not greater than 0.1%). The ion-acoustic wave density, having a high saturation value, determines the optical depth, which reaches unity within a few meters. The brightness temperature is thus entirely given by the level of Langmuir waves. These waves may be produced by trapped non-thermal electrons from previous burst sources. The same population also provides sufficient plasma waves for the type I continuum, which may arise from interactions with low-frequency waves present in the corona during times of type I activity.

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