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Solar cycle variations of anomalous ^4He as deduced by studies of cosmic ray ^3He

Cummings, A. C. and Mewaldt, R. A. and Stone, E. C. (1986) Solar cycle variations of anomalous ^4He as deduced by studies of cosmic ray ^3He. Geophysical Research Letters, 13 (10). pp. 1043-1046. ISSN 0094-8276. doi:10.1029/GL013i010p01043.

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Voyager 1 and 2 observations have been used to derive the energy spectrum of ‘anomalous’ cosmic ray (ACR) helium using a technique based on the separation of the isotopes of He. Previously reported observations show that the ACR oxygen spectrum underwent a change in shape following the solar magnetic field reversal in 1980; in this paper we present evidence for a corresponding change in the ACR helium spectrum. We find that the energy spectra of ACR helium and oxygen and galactic cosmic ray (GCR) ^4He and ^3He can be reproduced both before and after the field reversal using a simple solar modulation model in which the effects of curvature and gradient drifts are arbitrarily neglected.

Item Type:Article
Related URLs:
URLURL TypeDescription DOIArticle
Cummings, A. C.0000-0002-3840-7696
Mewaldt, R. A.0000-0003-2178-9111
Stone, E. C.0000-0002-2010-5462
Additional Information:© 1986 by the American Geophysical Union. Received July 31, 1986; Accepted August 26, 1986. We are grateful to R.E. Vogt for his contributions during his tenure as principal investigator for the Voyager CRS. We also appreciate the contributions of the other Voyager CRS team members at Caltech, Goddard Space Flight Center, and the Universities of Arizona and New Hampshire. This work was supported in part by NASA under contracts NAS 7-918 and NAG5-722, and grant NGR 05-002-160.
Group:Space Radiation Laboratory
Funding AgencyGrant Number
NASANGR 05-002-160
Issue or Number:10
Record Number:CaltechAUTHORS:20140219-103051736
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Usage Policy:No commercial reproduction, distribution, display or performance rights in this work are provided.
ID Code:43873
Deposited By: Tony Diaz
Deposited On:25 Feb 2014 21:05
Last Modified:10 Nov 2021 16:44

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