Estimation of coronal magnetic fields using Type-I emission

Details Estimation of coronal magnetic fields using Type-I emission Estimation of coronal magnetic fields using Type-I emission

Mar 1986

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1986baicz..37..115g&link_type=abstract

Astronomical Institutes of Czechoslovakia, Bulletin (ISSN 0004-6248), vol. 37, March 1986, p. 115-120.

Astronomy and Astrophysics

Astronomy

5

Coronal Loops, Solar Corona, Solar Magnetic Field, Solar Radio Bursts, Propagation Velocity, Radial Distribution, Rankine-Hugoniot Relation, Shock Wave Propagation, Solar Activity

Scientific paper

The radial dependence of the coronal magnetic field above active regions is calculated using Type-I chain data existing in the literature. Assuming that Type-I emission is due to shock waves, the upstream shock velocity and the density jump across the shock are obtained respectively from the drift rate and the bandwidth of the Type-I chains. Making use of the shock velocity and the density jump in the Rankine-Hugoniot relation, the Alfvén velocity and hence the magnetic field in the corona is calculated. The results are compared with existing estimates.

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