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Cosmic Ray Source Abundances Derived from High Energy Measurements of Fe-Group Nuclei

Mewaldt, R. A. and Webber, W. R. (1990) Cosmic Ray Source Abundances Derived from High Energy Measurements of Fe-Group Nuclei. In: Proceedings of the 21st International Cosmic Ray Conference. Vol.3. University of Adelaide , Northfield, South Australia, pp. 432-435. http://resolver.caltech.edu/CaltechAUTHORS:20140714-162316365

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Abstract

We examine the cosmic ray source composition of elements from Ar to Ni (18≤ Z≤28) using data from ~0.l to ~200 GeV /nuc and a cosmic ray propagation code that includes improved fragmentation cross-sections. By fitting available satellite data over more than three decades in energy /nuc, including recent HEA0-3 data, we obtain improved source abundances for Ar, Ca, Cr, Mn, and Ni, and compare these with recent determinations of the solar composition. We find no evidence for an energy-dependent source composition below ~20 GeV/nuc, but the data at higher energies deserve further study.


Item Type:Book Section
Related URLs:
URLURL TypeDescription
http://adslabs.org/adsabs/abs/1990ICRC....3..432M/ADSArticle
Additional Information:© Organizing Committee of the 21st Int. Cosmic Ray Conference. Provided by the NASA Astrophysics Data System. This work was supported by NASA grants NAG8-678 and NCR 05-002-160. We appreciate discussions of HEAO data with W. R. Binns, T. L. Garrard, J. Klarmann, and C. J. Waddington, and help with the propagation code from B. T. Hayes.
Group:Space Radiation Laboratory
Funders:
Funding AgencyGrant Number
NASANAG8-678
NASANCR 05-002-160
Other Numbering System:
Other Numbering System NameOther Numbering System ID
Space Radiation Laboratory1989-23
Record Number:CaltechAUTHORS:20140714-162316365
Persistent URL:http://resolver.caltech.edu/CaltechAUTHORS:20140714-162316365
Usage Policy:No commercial reproduction, distribution, display or performance rights in this work are provided.
ID Code:47199
Collection:CaltechAUTHORS
Deposited By: Deborah Miles
Deposited On:15 Jul 2014 16:15
Last Modified:15 Jul 2014 16:15

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