E-Print Archive

There are 3775 abstracts currently viewable.


Advanced Search
Main Page Add New E-Print Submitter
News Help/FAQ About Preferences
Manage Key Phrase
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 

Go to main E-Print pageGo to main E-Print page.
Previous AbstractPrevious Abstract.
Next AbstractNext Abstract.
Download PreprintDownload Preprint.
Submitter's HomepageSubmitters Homepage.
Edit EntryEdit Entry.
View All Abstracts By SubmitterView all abstracts by submitter.
Delete AbstractDelete abstract.

Latest Entries
A Statistical Analysis of the Solar Phenomena Associated with Global EUV Waves
Imaging Spectroscopy of Solar Radio Burst Fine Structures
On a small-scale EUV wave: the driving mechanism and the associated oscillating filament
Type III Solar Radio Burst Source Region Splitting Due to a Quasi-Separatrix Layer
On a solar blowout jet: driven mechanism and the formation of cool and hot components
Understanding the Role of Mass-Unloading in Filament Eruptions
Surges and Si IV bursts in the solar atmosphere. Understanding IRIS and SST observations through RMHD experiments
The direct relation between the duration of magnetic reconnection and the evolution of GOES light curves in solar flares
Large-Amplitude Longitudinal Oscillations Triggered by the Merging of Two Solar Filaments: Observations and Magnetic Field Analysis
Statistical Study of Solar White-light Flares and Comparisons with Superflares on Solar-type Stars
Effect of local thermal equilibrium misbalance on long-wavelength slow magnetoacoustic waves
Characteristics of Sustained >100 γ-ray Emission Associated with Solar Flares
Characteristics that Produce White-Light Enhancements in Solar Flares Observed by Hinode/SOT
Solar Energetic Particle Forecasting Algorithms and Associated False Alarms
Magnetic swirls and associated fast magnetoacoustic kink waves in a solar chromospheric flux tube
High-wavenumber solar f-mode strengthening prior to active region formation
Block-induced complex structures building the flare-productive solar active region 12673
Reconstruction of a Large-scale Pre-flare Coronal Current Sheet Associated with an Homologous X-shaped Flare
Comparison of Two Coronal Magnetic Field Models for Reconstructing a Sigmoidal Solar Active Region With Coronal Loops
A Magnetic Bald-Patch Flare in Solar Active Region 11117

Related Pages
MSU Solar Physics.
Max Millennium Science Mail Archive.
Max Millennium Message of the Day Mail Archive.
Max Millennium Flare Catalog

Archive Maintainer
Alisdair Davey

© 2003 Solar Physics Group - Montana State University