Solar-type U bursts and coronal transients

Details Solar-type U bursts and coronal transients Solar-type U bursts and coronal transients

Jul 1983

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1983a%26a...123..307l&link_type=abstract

Astronomy and Astrophysics (ISSN 0004-6361), vol. 123, no. 2, July 1983, p. 307-315.

Astronomy and Astrophysics

Astrophysics

17

Coronal Loops, Solar Electrons, Solar Magnetic Field, Solar Radio Bursts, Electron Acceleration, Electron Density (Concentration), Frequency Shift, Magnetic Field Configurations, Magnetically Trapped Particles, Spectroheliographs

Scientific paper

Solar type U bursts have been observed at Nancay with high sensitivity and large bandwidth instrumentation (470-150 MHz and 75-25 MHz). It is found that inside each group the turning frequency statistically decreases at a rate typical of coronal transient speeds. Moreover some events clearly show the association type I-type U bursts, both emissions drifting towards low frequencies. This confirms the model proposed by Leblanc and Aubier (1977) and Aubier et al. (1978), the same electrons giving rise successively to both burst types. This occurs in particular when the magnetic field cross section increases upwards as it is the case in transient loops. The conclusion is that type Us preferentially occur in transient loops and these drifting type U bursts are the direct radio evidence of the ejection of a magnetic arch in the corona. These events provide us with the density evolution: it is found that the electron density inside an expanding arch decreases faster at the top than at the foot.

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