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Cosmic Ray Source Abundances for 29≤Z≤34

George, J. S. and Binns, W. R. and Christian, E. R. and Cummings, A. C. and Hink, P. L. and Klarmann, J. and Leske, R. A. and Lijowski, M. and Mewaldt, R. A. and Stone, E. C. and von Rosenvinge, T. T. and Wiedenbeck, M. E. and Yanasak, N. E. (1999) Cosmic Ray Source Abundances for 29≤Z≤34. In: Proceedings of the 26th International Cosmic Ray Conference. Vol.3. International Union of Pure and Applied Physics , pp. 13-16.

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The Cosmic Ray Isotope Spectrometer (CRIS) instrument on board the Advanced Composition Explorer (ACE) spacecraft is making new measurements of nuclides just beyond the iron-nickel peak in the galactic cosmic rays. Isotopes of copper and zinc have been resolved for the first time. Elemental abundances for nuclei with 29≤Z≤34 are reported with good separation between species. Several of these elements are useful for studying fractionation processes which may depend on the first ionization potential or volatility. Source abundances are estimated using a prior propagation calculation and their potential for distinguishing between source models are discussed.

Item Type:Book Section
Related URLs:
URLURL TypeDescription
Binns, W. R.0000-0001-6110-3407
Christian, E. R.0000-0003-2134-3937
Cummings, A. C.0000-0002-3840-7696
Leske, R. A.0000-0002-0156-2414
Mewaldt, R. A.0000-0003-2178-9111
Stone, E. C.0000-0002-2010-5462
Wiedenbeck, M. E.0000-0002-2825-3128
Additional Information:© University of Utah. Provided by the NASA Astrophysics Data System. This work was supported by NASA at the California Institute of Technology (under grant NAG5-6912), the Jet Propulsion Laboratory, the Goddard Space Flight Center, and Washington University.
Group:Space Radiation Laboratory
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Other Numbering System NameOther Numbering System ID
Space Radiation Laboratory1999-27
Record Number:CaltechAUTHORS:20150213-092825276
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Usage Policy:No commercial reproduction, distribution, display or performance rights in this work are provided.
ID Code:54819
Deposited By: Deborah Miles
Deposited On:13 Feb 2015 21:06
Last Modified:09 Mar 2020 13:19

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