E-Print Archive

There are 3873 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
The Solar Photospheric-to-Coronal Fe abundance from X-ray Fluorescence Lines View all abstracts by submitter

Kenneth Phillips   Submitted: 2012-01-03 05:44

The ratio of the Fe abundance in the photosphere to that in coronal flare plasmas is determined by X-ray lines within the complex at 6.7 keV (1.9~AA) emitted during flares. The line complex includes the He-like Fe (fexxv) resonance line w (6.70 keV) and Fe K α lines (6.39, 6.40 keV), the latter being primarily formed by the fluorescence of photospheric material by X-rays from the hot flare plasma. The ratio of the Fe K α lines to the fexxv w depends on the ratio of the photospheric-to-flare Fe abundance, heliocentric angle heta of the flare, and the temperature Te of the flaring plasma. Using high-resolution spectra from X-ray spectrometers on the {em P78-1} and {em Solar Maximum Mission} spacecraft, the Fe abundance in flares is estimated to be 1.6pm 0.5 and 2.0 pm 0.3 times the photospheric Fe abundance, the {em P78-1} value being preferred as it is more directly determined. This enhancement is consistent with results from X-ray spectra from the {em RHESSI} spacecraft, but is significantly less than a factor 4 as in previous work.

Authors: K. J. H. Phillips
Projects: Yohkoh-BCS

Publication Status: Accepted by MNRAS
Last Modified: 2012-01-03 08:25
Go to main E-Print page  Wave-particle interactions in non-uniform plasma and the interpretation of Hard X-ray spectra in solar flares  Heating of Flare Loops With Observationally Constrained Heating Functions  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
Time resolved spectroscopic observations of an M-dwarf flare star EV Lac during a flare
Two Episodes of Magnetic Reconnections During a Confined Circular-ribbon Flare
Enhanced stellar activity for slow antisolar differential rotation?
Quasi-periodic pulsations in the most powerful solar flare of Cycle 24
GONG Catalog of Solar Filament Oscillations Near Solar Maximum
Chromospheric response during the precursor and the main phase of a B6.4 flare on August 20, 2005
Unambiguous Evidence of Coronal Implosions During Solar Eruptions and Flares
Two Types of Long-duration Quasi-static Evolution of Solar Filaments
Oscillations of cometary tails: a vortex shedding phenomenon?
Observations of Running Penumbral Waves Emerging in a Sunspot
Reconnection in the Post-Impulsive Phase of Solar Flares
Temperature of source regions of 3He-rich impulsive solar energetic particles events
3He-rich Solar Energetic Particles in Helical Jets on the Sun
On the importance of the nonequilibrium ionization of Si IV and O IV and the line-of-sight in solar surges
Was the cosmic ray burst detected by the GRAPES-3 on 22 June 2015 caused by transient weakening of geomagnetic field or by an interplanetary anisotropy?
Connecting Coronal Mass Ejections to Their Solar Active Region Sources: Combining Results from the HELCATS and FLARECAST Projects
Studies of Isolated and Non-isolated Photospheric Bright Points in an Active Region Observed by the New Vacuum Solar Telescope
Fermi-LAT observations of the 2017 September 10th solar flare
Propagation of a global coronal wave and its interaction with large-scale coronal magnetic structures
A New Tool for CME Arrival Time Prediction Using Machine Learning Algorithms: CAT-PUMA

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