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The Time History of 2.22 MeV Line Emission in Solar Flares

Prince, T. A. and Forrest, D. J. and Chupp, E. L. and Kanbach, G. and Share, G. H. (1983) The Time History of 2.22 MeV Line Emission in Solar Flares. In: 18th International Cosmic Ray Conference, Bangalore, India, August 22 to September 3, 1983. Vol.4. Tata Institute of Fundamental Research , Bombay, India, pp. 79-82. https://resolver.caltech.edu/CaltechAUTHORS:20140423-134935332

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Abstract

In this paper we examine the time dependence of 2.22 MeV emission using observations of the Solar Maximum Mission (SMM) gamma-ray spectrometer. We will determine the decay time constant for the 2.22 MeV emission process and from this derive implications concerning the density at which neutrons are captured and the value of the ^3He/H ratio. We will also set upper limits on the number of low energy neutrons produced in solar flares. The 2.22 MeV line provides a unique tool for probing the physics of the solar atmosphere since the neutrons which produce the line penetrate to depths exceeding the opacities at which optical observations can be made.


Item Type:Book Section
Related URLs:
URLURL TypeDescription
http://adsabs.harvard.edu/abs/1983ICRC....4...79PADSArticle
ORCID:
AuthorORCID
Prince, T. A.0000-0002-8850-3627
Contact Email Address:dmiles@caltech.edu
Group:Space Radiation Laboratory
Other Numbering System:
Other Numbering System NameOther Numbering System ID
Space Radiation Laboratory1983-11
Record Number:CaltechAUTHORS:20140423-134935332
Persistent URL:https://resolver.caltech.edu/CaltechAUTHORS:20140423-134935332
Usage Policy:No commercial reproduction, distribution, display or performance rights in this work are provided.
ID Code:45160
Collection:CaltechAUTHORS
Deposited By: SWORD User
Deposited On:24 Apr 2014 22:47
Last Modified:03 Oct 2019 06:27

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