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Measurement of Vector Magnetic Field in a Flare kernel with a Spectropolarimetric Observation in He I 10830 A View all abstracts by submitter

Tetsu Anan   Submitted: 2018-08-27 15:03

A flare kernel associated with a C4 class flare was observed in a spectral window including the He I triplet 10830 Å and Si I 10827 Å with a spectropolarimeter on the Domeless Solar Telescope at Hida Observatory on August 9th, 2015. Observed Stokes profiles of the He I triplet in the flare kernel in its post-maximum phase are well reproduced through inversions considering the Zeeman and the Paschen-Back effects with a three slab model of the flare kernel, in which two slabs having up and downward velocities produce emissions and one slab produces an absorption. The magnetic field strength inferred from the emission components of the He I line is 1400 G, which is significantly stronger than 690 G that is observed at the same location in the same line 6.5 hours before the flare. In addition, photospheric magnetic field vector derived from the Si I 10827 Å is similar to that of the flare kernel. To explain this results, we suggest that the emission in the He I triplet during the flare is produced in the deep layer, around which bombardment of non-thermal electrons leads to the formation of a coronal temperature plasma. Assuming a hydrogen column density at the location where the He I emissions are formed, and a power-law index of non-thermal electron energy distribution, we derived the low-energy cutoff of the non-thermal electron as 20 - 30 keV, which is consistent with that inferred from hard X-ray data obtained by RHESSI.

Authors: Tetsu Anan, Takurou Yoneya, Kiyoshi Ichimoto, Satoru Ueno, Daikou Shiota, Satoshi Nozawa, Shinsuke Takasao, Tomoko Kawate
Projects: Domeless Solar Telescope (Hida Observatory)

Publication Status: accepted for publication in PASJ
Last Modified: 2018-08-31 12:55
Go to main E-Print page  Coronal condensations caused by magnetic reconnection between solar coronal loops  The Relation Between Escape and Scattering Times of Energetic Particles in a Turbulent Magnetized Plasma: Application to Solar Flares  Edit Entry  Download Preprint  Delete Entry 

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