Heating of Erupting Prominences Observed at 17 GHZ

Details Heating of Erupting Prominences Observed at 17 GHZ Heating of Erupting Prominences Observed at 17 GHZ

Jan 1999

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1999apj...510..466h&link_type=abstract

The Astrophysical Journal, Volume 510, Issue 1, pp. 466-473.

Astronomy and Astrophysics

Astronomy

14

Sun: Flares, Sun: Prominences, Sun: Radio Radiation

Scientific paper

We have found evidence that heating of erupting prominences occurs at the beginning of two events on 1992 November 5 and 1994 February 20, which were observed with the Nobeyama Radioheliograph at 17 GHz. Both of the events are eruptions of prominences on the disk, which are seen as eruptions of dark filaments. The radio images of the events show very similar changes. Shortly after the filaments begin to be accelerated rapidly and detach from the disk, the filaments apparently disappear. However, when the moving filaments pass above bright plage regions, the plage regions become dark. These facts indicate that the brightness temperature of the dark filaments increases to the temperature of the quiet disk at the beginning of the abrupt eruptions, while the filaments keep their large optical thickness. After the rapid increase, the brightness temperature does not change significantly during the motion of the filaments. In contrast to Hα, the visibility of prominences in 17 GHz images is not affected by Doppler shifts. Therefore, changes in the brightness temperature reflect changes in the physical parameters of prominences. Heating of the surface of the cool core of the prominences up to the transition-region temperature is the most plausible explanation of the observed increase in the brightness temperature at 17 GHz.

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