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Unusual Enhancements of MeV Ions and Electrons as Voyager 1 Approaches the Heliospheric Termination Shock

McDonald, F. B. and Cummings, A. C. and Stone, E. C. and Heikkila, B. and Lal, N. and Webber, W. R. (2003) Unusual Enhancements of MeV Ions and Electrons as Voyager 1 Approaches the Heliospheric Termination Shock. In: Proceedings of the 28th International Cosmic Ray Conference. Vol.7. International Union of Pure and Applied Physics , Tokyo, Japan, pp. 3765-3768. https://resolver.caltech.edu/CaltechAUTHORS:20150306-111608994

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Abstract

In mid-2002 as Voyager 1 moved beyond 85 AU there began an unusual increase of 2.5 MeV ions that remained at a level near 0.1 protons/cm^2-s-sr-MeV for some 6 months. Simultaneously there was an increase in the 2.5 - 70 MeV electrons and in the galactic and anomalous cosmic ray intensity. The electrons are most probably of galactic origin and like the cosmic ray ions are responding to the more favorable modulation levels in the distant heliosphere. It is proposed that the MeV ions are of solar/interplanetary (S/IP) origin with possibly a significant component of IP accelerated pickup ions that have been reaccelerated. Several possibilities for this reacceleration are discussed including the proximity of the termination shock (T.S.).


Item Type:Book Section
Related URLs:
URLURL TypeDescription
http://adsabs.harvard.edu/abs/2003ICRC....7.3765MADSArticle
ORCID:
AuthorORCID
Cummings, A. C.0000-0002-3840-7696
Stone, E. C.0000-0002-2010-5462
Additional Information:Copyright 2003 by Universal Academy Press, Inc.
Group:Space Radiation Laboratory
Other Numbering System:
Other Numbering System NameOther Numbering System ID
Space Radiation Laboratory2003-34
Record Number:CaltechAUTHORS:20150306-111608994
Persistent URL:https://resolver.caltech.edu/CaltechAUTHORS:20150306-111608994
Usage Policy:No commercial reproduction, distribution, display or performance rights in this work are provided.
ID Code:55594
Collection:CaltechAUTHORS
Deposited By: Deborah Miles
Deposited On:17 Mar 2015 02:12
Last Modified:20 Feb 2020 14:33

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