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The relationship of energy flow at the magnetopause to geomagnetic activity

Baker, D. N. and Stone, E. C. (1977) The relationship of energy flow at the magnetopause to geomagnetic activity. Geophysical Research Letters, 4 (10). pp. 395-398. ISSN 0094-8276. http://resolver.caltech.edu/CaltechAUTHORS:20140204-144256426

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Abstract

Properties of the energetic electron (E ≳ 200 keV) magnetopause layer along the distant magnetotail have been studied with Caltech instrumentation aboard IMP-8 for approximately 60 spacecraft orbits. The cross-sectional area of the layer appears to increase by a factor of ∼ 5 with increasing geomagnetic activity, and the average unidirectional electron flux within the layer increases by a factor of ∼ 4. The energy carried by electrons ≳ 200 keV ranges from ∼ 10^(14) ergs sec^(−1) to ∼ 10^(15) ergs sec^(−1). Extrapolation to include all electrons > 1 keV suggests total energy flow ranging from ∼ 3×10^(15) ergs sec^(−1) at quiet times to ∼ 5×10^(18) ergs sec^(−1) at magnetically disturbed times.


Item Type:Article
Related URLs:
URLURL TypeDescription
http://dx.doi.org/10.1029/GL004i010p00395DOIArticle
http://onlinelibrary.wiley.com/doi/10.1029/GL004i010p00395/abstractPublisherArticle
Additional Information:© 1977 by the American Geophysical Union. Manuscript Accepted: 11 Aug 1977. Manuscript Received: 29 Jul 1977. This work was supported in part by the National Aeronautics and Space Administration under contract NAS5-11066 and Grant NGR0 5-002-160.
Group:Space Radiation Laboratory
Funders:
Funding AgencyGrant Number
NASANAS5-11066
NASANGR 05-002-160
Other Numbering System:
Other Numbering System NameOther Numbering System ID
Space Radiation Laboratory1977-04
Record Number:CaltechAUTHORS:20140204-144256426
Persistent URL:http://resolver.caltech.edu/CaltechAUTHORS:20140204-144256426
Usage Policy:No commercial reproduction, distribution, display or performance rights in this work are provided.
ID Code:43657
Collection:CaltechAUTHORS
Deposited By: Ruth Sustaita
Deposited On:04 Feb 2014 23:05
Last Modified:13 Feb 2019 18:05

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