Microwave, Optical, EUV, and Hard X-Ray Signature of Possible Coronal Loop Interaction

Details Microwave, Optical, EUV, and Hard X-Ray Signature of Possible Coronal Loop Interaction Microwave, Optical, EUV, and Hard X-Ray Signature of Possible Coronal Loop Interaction

Jul 2005

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2005soph..229..227h&link_type=abstract

Solar Physics, Volume 229, Issue 2, pp.227-236

Physics

7

Scientific paper

In this paper, we present a comprehensive picture for the M2.0 class flare of September 9, 2002 with an extensive multi-wavelength analysis. The flare was observed by the Ramaty High Energy Solar Spectroscopic Imager (RHESSI), the Owens Valley Solar Arrays (OVSA), and Big Bear Solar Observatory (BBSO). At BBSO, the observation was specially made at the wavelength of Hα - 1.3 Å with a cadence of ˜40 ms. For this multi-kernel flare, we find two pairs of conjugate kernels. Each pair has its centroid separation curve, which is well correlated with its own optical light curve. This clearly indicates two separate energy releasing sites. The proposed picture of the two energy release sites is supported by double peaks in microwave profiles, and, especially, the presence of two different 195 Å flaring loops observed by the Extreme UV Imaging Telescope (EIT) on board the Solar and Heliospheric Observatory (SOHO). Nevertheless, the two pairs surely have some intrinsic relations, which are indicated from both temporal and spatial correlations. Because of the intimate relationship, we propose that the two loop systems were interacting during the flare. In addition, one of the most pronounced features of this multi-kernel flare is that the results from microwaves are poorly correlated with those from hard X-ray (HXR) and optical data. The discrepancy is shown in two aspects: time profiles as well as emission locations. We still cannot understand the cause of the discrepancy, except that the interacting loops may have complicated the situation.

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