Nobeyama Radioheliograph and RHESSI Observations of the X1.5 Flare of 2002 April 21

Details Nobeyama Radioheliograph and RHESSI Observations of the X1.5 Flare of 2002 April 21 Nobeyama Radioheliograph and RHESSI Observations of the X1.5 Flare of 2002 April 21

Jan 2004

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2004apj...600.1052k&link_type=abstract

The Astrophysical Journal, Volume 600, Issue 2, pp. 1052-1060.

Astronomy and Astrophysics

Astronomy

11

Sun: Corona, Sun: Flares, Sun: Radio Radiation

Scientific paper

We present an overview of the radio observations of the X1.5 flare of 2002 April 21 and complementary data from other wavelengths. This flare was fairly well observed by the Ramaty High Energy Spectroscopic Imager (RHESSI) spacecraft and fully observed by the Nobeyama Radioheliograph (NoRH) at 17 and 34 GHz. This long-duration event lasted more than 2 hr and featured a beautiful arcade of rising loops on the limb visible at X-ray, EUV, and radio wavelengths. The main flare was preceded by a small event 90 minutes earlier showing a long EUV loop connecting well-separated radio and hard X-ray sources. The main flare itself starts with a compact radio and hard X-ray source at the eastern end of the region that develops into emission close to the solar surface (and well inside the solar limb) over a large region to the northwest. As the flare proceeds, a large set of loops is seen to rise well above the solar limb. Distinct regions of radio emission with very different time behavior can be identified in the radio images, and, in particular, a peculiar nonthermal source seen in radio and hard X-rays low in the corona at the base of the arcade is seen to turn on 30 minutes after the start of the impulsive phase. At about the same time, an extremely intense burst of coherent radio emission is seen from 500 to 2000 MHz; we speculate that this lower-frequency burst is produced by electrons that are accelerated in the nonthermal source at the base of the arcade and injected into the loop system where they radiate plasma emission in the 1010 cm-3 density plasma at the top of the arcade of loops. This event is striking as a demonstration of the many ways in which a flare can produce radio emission, and the combined data at different wavelengths reveal a diversity of energy release and nonthermal acceleration sites.

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