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White-light Emission and Chromospheric Response by an X1.8-class Flare on 2012 October 23 View all abstracts by submitter

Kyoko Watanabe   Submitted: 2020-03-11 01:19

On 2012 October 23, a strong white-light emission, associated with an X1.8-class flare, was observed by the Solar Optical Telescope on board the Hinode satellite. White-light kernels were clearly observed along the Ca II H ribbons. RHESSI also observed hard X-ray emissions that were almost located on the white-light kernels. The total energy of the white-light emission was ~1027-28 erg s-1 and the total energy of the accelerated electrons was almost of the same order when we used 40 keV as the lower energy cutoff. The white-light emission appears to have originated from nonthermal electrons in these energies. Moreover, the EUV imaging spectrometer on board the Hinode satellite performed a raster scan over this flaring active region and the flare occurred during the scan. Over the white-light kernels, we observed redshifts of a few tens of km s-1 in Fe XII. It appears that these EUV responses originated from some accelerated electrons due to the solar flare and they are considered to be the source of the white-light emission. In fact, the electron density of the white-light kernels was less than 1012 cm-3, which is sufficiently low for nonthermal electrons to penetrate into the photosphere.

Authors: Kyoko Watanabe and Shinsuke Imada
Projects: GOES X-rays,Hinode/EIS,Hinode/SOT,RHESSI,SDO-AIA,SDO-HMI

Publication Status: The Astrophysical Journal, Volume 891, Issue 1, id.88 (8pp)
Last Modified: 2020-03-11 13:14
Go to main E-Print page  Properties of ICME-Induced Forbush decreases at Earth and Mars  Helicity and winding fluxes as indicators of twisted flux emergence  Edit Entry  Download Preprint  Delete Entry 

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