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Time variations of observed Hα line profiles and precipitation depths of non-thermal electrons in a solar flare View all abstracts by submitter

Robert Falewicz   Submitted: 2017-09-01 03:20

We compare time variations of the Hα and X-ray emissions observed during the pre-impulsive and impulsive phases of the C1.1-class solar flare on 21 June 2013 with those of plasma parameters and synthesized X-ray emission from a one-dimensional hydro-dynamic numerical model of the flare. The numerical model was calculated assuming that the external energy is delivered to the flaring loop by non-thermal electrons. The Hα spectra and images were obtained using the Multi-channel Subtractive Double Pass spectrograph with a time resolution of 50~ms. The X-ray fluxes and spectra were recorded by the Reuven Ramaty High-Energy Solar Spectroscopic Imager ( RHESSI). Pre-flare geometric and thermodynamic parameters of the model and the delivered energy were estimated using RHESSI data. The time variations of the X-ray light curves in various energy bands and the those of the Hα intensities and line profiles were well correlated. The time scales of the observed variations agree with the calculated variations of the plasma parameters in the flaring loop footpoints, reflecting the time variations of the vertical extent of the energy deposition layer. Our result shows that the fast time variations of the Hα emission of the flaring kernels can be explained by momentary changes of the deposited energy flux and the variations of the penetration depths of the non-thermal electrons.

Authors: R. Falewicz, K. Radziszewski, P. Rudawy, A. Berlicki
Projects: None

Publication Status: accepted to ApJ
Last Modified: 2017-09-01 11:13
Go to main E-Print page  Spectroscopy of Very Hot Plasma in Non-flaring Parts of a Solar Limb Active Region: Spatial and Temporal Properties  A Solar cycle correlation of coronal element abundances in Sun-as-a-star observations  Edit Entry  Download Preprint  Delete Entry 

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