Storms of U-bursts and the stability of coronal loops

Details Storms of U-bursts and the stability of coronal loops Storms of U-bursts and the stability of coronal loops

Feb 1985

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1985a%26a...143..365l&link_type=abstract

Astronomy and Astrophysics (ISSN 0004-6361), vol. 143, no. 2, Feb. 1985, p. 365-373.

Physics

Plasma Physics

8

Coronal Loops, Plasma Physics, Solar Magnetic Field, Solar Prominences, Solar Radio Bursts, Solar Storms, Plasma Acceleration, Solar Wind, Type 2 Bursts, Type 3 Bursts

Scientific paper

U-burst activity as observed in the frequency range of 25-75 MHz with the large array and sweep frequency spectrograph of Nancay, is analyzed by using five years of observations. In this frequency range, U-bursts sometimes occur isolated but most often in groups and in storms; in this case U-bursts are generally inverted J or L-shaped. Evidence is shown for a close relationship between Type II events and U-burst groups, and that several Type II bursts occurred during Type III-U storms. It is concluded that the existence of frequent U-burst storms implies large magnetic arches stable for as long as a few days and that these arches are very probably diverging to explain J and L-shaped bursts. The association of Type II events and U-burst activity is interpreted as a result of coronal mass ejections which are responsible for transient loops.

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