E-Print Archive

There are 4002 abstracts currently viewable.


Search:

Advanced Search
Options
Main Page Add New E-Print Submitter
Information
Feedback
News Help/FAQ About Preferences
Manage Key Phrase
Notification
Spectral Characteristics of Solar Flares in Different Chromospheric Lines and Their Implications View all abstracts by submitter

Hui Li   Submitted: 2007-02-25 22:46

Using the spectral data of representative solar ares observed with the infrared detector system of the solar spectrograph at Purple Mountain Observatory, we study the spectroscopic characteristics of solar ares in the Hα , the CaII 8542 and the HeI 10830 lines in different phases and various locations of ares, and discuss their possible implications in couple with space observations. Our results show that in the initial phase of a are the Hα line displays red-shift only and no wide-wing. Large broadenings of the Hα line are observed in a few minutes after the are onset within small regions of 3'' - 5'' in both disk and limb ares with/without non-thermal processes. Far wings similar to those of damping roadening appear not only in the Hα line but in the HeI 10830 line as well in ares with non-thermal processes. Sometimes we even detect weak far-wing emission in the CaII 8542 line in disk ares. Such large broadenings are observed in both the footpoints and the are loop-top regions, and possibly result from strong turbulence and/or macroscopic motions. Therefore, the so-called 'non-thermal wing' of the Hα line prossile is not a suffcient condition to distinguish whether non-thermal electrons are accelerated or not in a flare. The CaII 8542 line shows lower intensity in the loop-top regions and higher intensity in the parts close to the solar surface. Emissions larger than nearby continuum in the HeI 10830 line are detected only in small regions with strong X-ray emissions and avoid sunspot umbrae.

Authors: Hui Li, Jianqi You, Xingfeng Yu and Qiusheng Du
Projects: None

Publication Status: Solar Physics, accepted.
Last Modified: 2007-02-26 11:04
Go to main E-Print page  Direct propagation of photospheric acoustic p-modes into non-magnetic solar atmosphere  Magnetic flux emergence in granular convection: Radiative MHD simulations and observational signatures  Edit Entry  Download Preprint  Submitter's Homepage Delete Entry 

Key
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
The Role of a Tiny Brightening in a Huge Geo-effective Solar Eruption Leading to the St Patrick's Day Storm
A basal contribution from p-modes to the Alfvénic wave flux in the corona
Multiwavelength Study of Equatorial Coronal-Hole Jets
Non-thermal hydrogen Lyman line and continuum emission in solar flares generated by electron beams
Determining normal mode features from numerical simulations using CEOF analysis: I. Test case using transverse oscillations of a magnetic slab
Modelling the Effect of Mass-Draining on Prominence Eruptions
Transverse waves in coronal flux tubes with thick boundaries: The effect of longitudinal flows
Electron distribution and energy release in magnetic reconnection outflow regions during the pre-impulsive phase of a solar flare
Benchmarking CME arrival time and impact: Progress on metadata, metrics, and events
First Unambiguous Imaging of Large-Scale Quasi-Periodic Extreme-Ultraviolet Wave or Shock
Coronal Imaging with the Solar UltraViolet Imager
Investigation of pre-flare dynamics using the weighted horizontal magnetic gradient method: From small to major flare classes
Seismological determination of the Alfvén speed and plasma-beta in solar photospheric bright points
Dynamo Wave Patterns Inside the Sun Revealed by Torsional Oscillations
Evidence of Twisting and Mixed-polarity Solar Photospheric Magnetic Field in Large Penumbral Jets: IRIS and Hinode Observations
Dissipation scale lengths of density turbulence in the inner solar wind
On the Possibility of Generating Harmonics of the Electron Plasma Frequency in the Solar Atmosphere due to Explosive Instability in a System of Interpenetrating Electron and Ion Flows
Determination of the total accelerated electron rate and power using solar flare hard X-ray spectra
Transition from axi- to nonaxisymmetric dynamo modes in spherical convection models of solar-like stars
Can high-mode magnetohydrodynamic waves propagating in a spinning macrospicule be unstable due to the Kelvin-Helmholtz instability?

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