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Cosmic-ray energy changes in the heliosphere. II. The effect on K-capture electron secondaries

Caballero-Lopez, R. A. and Moraal, H. and Mewaldt, R. A. and McDonald, F. B. and Wiedenbeck, M. E. (2007) Cosmic-ray energy changes in the heliosphere. II. The effect on K-capture electron secondaries. Astrophysical Journal, 663 (2). pp. 1335-1339. ISSN 0004-637X. doi:10.1086/518394.

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Recent accurate measurements of the cosmic-ray intensity ratio ^(51)V/^(51)Cr below 1 GeV nucleon^(-1) provide a powerful new tool to study cosmic-ray modulation in the heliosphere. This paper describes how energy changes during this modulation process influence this ratio. In particular, our model includes acceleration at the solar wind termination shock, and we find that this mechanism significantly enhances the ^(51)V/^(51)Cr ratio at 1 AU. It is also shown that this acceleration makes the ratio more sensitive to the form of local low-energy interstellar spectra, below ~100 MeV nucleon^(-1), than without it. Specifically, this acceleration provides an independent confirmation of the consensus that low-energy spectra should be flatter than their high-energy power-law forms.

Item Type:Article
Related URLs:
URLURL TypeDescription
Mewaldt, R. A.0000-0003-2178-9111
Wiedenbeck, M. E.0000-0002-2825-3128
Additional Information:© 2007 The American Astronomical Society. Received 2006 January 24; accepted 2007 March 22. This work was supported by UNAM-DGAPA grant IN106105 in Mexico, NSF grant ATM 0107181 at Maryland, NASA grant NAG5-12929 at Caltech and JPL, and the South African National Research Foundation.
Group:Space Radiation Laboratory
Funding AgencyGrant Number
NSFATM 0107181
South African National Research FoundationUNSPECIFIED
Subject Keywords:cosmic rays; Sun: particle emission
Issue or Number:2
Record Number:CaltechAUTHORS:CABapj07
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Usage Policy:No commercial reproduction, distribution, display or performance rights in this work are provided.
ID Code:13702
Deposited By: Tony Diaz
Deposited On:09 Jul 2009 18:18
Last Modified:08 Nov 2021 22:40

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