Coronal abundances and their variation
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Coronal abundances and their variation final report for contract NASW-4814 by

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Published by National Aeronautics and Space Administration, National Technical Information Service, distributor in [Washington, DC, Springfield, Va .
Written in English


  • Solar corona,
  • Abundance,
  • X ray spectra,
  • Line spectra

Book details:

Edition Notes

Statementprincipal investigator, Julia L.R. Saba.
Series[NASA contractor report] -- NASA-CR-203043., NASA contractor report -- NASA CR-203043.
ContributionsUnited States. National Aeronautics and Space Administration.
The Physical Object
Pagination1 v.
ID Numbers
Open LibraryOL17834309M

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coronal structure as observed with TRACE. Coronal observations derive from heavy-ion emission; thus, we focus on the extent to which flow may modify coronal abundances by examining the heavy-ion abundance stratification within long-lived loops. We discuss the magnitudes of the physical effects modeled and compare simulated results with. A coronal mass ejection (CME) is a significant release of plasma and accompanying magnetic field from the solar often follow solar flares and are normally present during a solar prominence eruption. The plasma is released into the solar wind, and can be observed in coronagraph imagery.. Coronal mass ejections are often associated with other forms of solar activity, but a broadly. Abundance enhancements of elements with 2≤Z≤56, relative to coronal abundances, show a power-law dependence versus their average mass-to-charge ratio A/Q, which varies from event to event and. We present measurements of relative elemental abundances in plumes and interplumes. Plumes are bright, narrow structures in coronal holes that extend along open magnetic field lines far out into the corona. Previous work has found that in some coronal structures the .

Open Library is an initiative of the Internet Archive, a (c)(3) non-profit, building a digital library of Internet sites and other cultural artifacts in digital projects include the Wayback Machine, and Sponsor a Book. Abundance 16 works Search for books with subject Abundance. Search. Coronal abundances and their variation Julia L. R. Saba Read. Read. Read. Accurate measurements of the local deuterium abundance from HST spectr J. L. Linsky Read. Timed Doppler Interferometer, TIDI. journal article: anomalous relative ar/ca coronal abundances observed by the hinode/euv imaging spectrometer near sunspots. Solar Energetic Particles: Sampling Coronal Abundances Fe/O) are enhanced relative to photospheric abundances and may vary around their respective coronal values. relative to coronal.

The Solar Abundances Conclusion We may conclude with the remark that the photospheric abundances are in general known at least to within a factor of two. For some of the elements the abundance uncertainty is even much smaller, as may be seen from the foregoing brief discussion. This includes the much discussed photospheric iron by: ACE/SWICS measurements for the Genesis collection period also show a continuum in compositional variation as a function of velocity for the quasi-stationary flow that defies the simple binning of samples into their sources of coronal hole (CH) and interstream (IS). • The chemical abundances measured in the intra-cluster plasma thus provide us with a fossil record of the integral yield of all the different stars (releasing metals in supernova explosions and winds) that have left their specific abundance patterns in the gas prior and during cluster evolution. Noname manuscript No. (will be inserted by the editor) Element abundances in X-ray emitting plasmas in stars Paola Testa arXivv1 [] 1 Dec Received: date / Accepted: date Abstract Studies of element abundances in stars are of fundamental interest for their impact in a wide astrophysical context, from our understanding of galactic chemistry and its evolution, to their.