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Global Energetics of Thirty-Eight Large Solar Eruptive Events

Emslie, A. G. and Dennis, B. R. and Shih, A. Y. and Chamberlin, P. C. and Mewaldt, R. A. and Moore, C. S. and Share, G. H. and Vourlidas, A. and Welsch, B. T. (2012) Global Energetics of Thirty-Eight Large Solar Eruptive Events. Astrophysical Journal, 759 (1). Art. No. 71. ISSN 0004-637X. https://resolver.caltech.edu/CaltechAUTHORS:20121218-082946002

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Abstract

We have evaluated the energetics of 38 solar eruptive events observed by a variety of spacecraft instruments between 2002 February and 2006 December, as accurately as the observations allow. The measured energetic components include: (1) the radiated energy in the Geostationary Operational Environmental Satellite 1-8 Å band, (2) the total energy radiated from the soft X-ray (SXR) emitting plasma, (3) the peak energy in the SXR-emitting plasma, (4) the bolometric radiated energy over the full duration of the event, (5) the energy in flare-accelerated electrons above 20 keV and in flare-accelerated ions above 1 MeV, (6) the kinetic and potential energies of the coronal mass ejection (CME), (7) the energy in solar energetic particles (SEPs) observed in interplanetary space, and (8) the amount of free (non-potential) magnetic energy estimated to be available in the pertinent active region. Major conclusions include: (1) the energy radiated by the SXR-emitting plasma exceeds, by about half an order of magnitude, the peak energy content of the thermal plasma that produces this radiation; (2) the energy content in flare-accelerated electrons and ions is sufficient to supply the bolometric energy radiated across all wavelengths throughout the event; (3) the energy contents of flare-accelerated electrons and ions are comparable; (4) the energy in SEPs is typically a few percent of the CME kinetic energy (measured in the rest frame of the solar wind); and (5) the available magnetic energy is sufficient to power the CME, the flare-accelerated particles, and the hot thermal plasma.


Item Type:Article
Related URLs:
URLURL TypeDescription
http://dx.doi.org/10.1088/0004-637X/759/1/71DOIUNSPECIFIED
http://iopscience.iop.org/0004-637X/759/1/71PublisherUNSPECIFIED
ORCID:
AuthorORCID
Mewaldt, R. A.0000-0003-2178-9111
Vourlidas, A.0000-0002-8164-5948
Additional Information:© 2012 American Astronomical Society. Received 2012 July 1; accepted 2012 September 17; published 2012 October 17. We thank Gordon Holman, Richard Schwartz, and Kim Tolbert for help with analyzing the GOES and RHESSI data, and Anil Gopie for doing most of the GOES data analysis. We also thank the referee for an unusually comprehensive and thorough review of the originally submitted version of this manuscript, which resulted in a significantly improved paper. A.G.E. was supported by NASA Grant NNX10AT78J, R.A.M. by NASA Grants NNX08AI11G and NNX11AO75G, and A.V. by various NASA grants to the Naval Research Laboratory. SOHO is a joint ESA and NASA mission. CHIANTI is a collaborative project involving researchers at NRL (USA), RAL (UK), and the Universities of Cambridge (UK), George Mason (USA), and Florence (Italy).
Group:Space Radiation Laboratory
Funders:
Funding AgencyGrant Number
NASANNX10AT78J
NASANNX08AI11G
NASANNX11AO75G
NASAUNSPECIFIED
Subject Keywords:Sun: activity; Sun: coronal mass ejections (CMEs); Sun: flares; Sun: particle emission; Sun: X-rays, gamma rays
Other Numbering System:
Other Numbering System NameOther Numbering System ID
Space Radiation Laboratory2012-13
Issue or Number:1
Record Number:CaltechAUTHORS:20121218-082946002
Persistent URL:https://resolver.caltech.edu/CaltechAUTHORS:20121218-082946002
Official Citation:Global Energetics of Thirty-eight Large Solar Eruptive Events A. G. Emslie, B. R. Dennis, A. Y. Shih, P. C. Chamberlin, R. A. Mewaldt, C. S. Moore, G. H. Share, A. Vourlidas, and B. T. Welsch doi:10.1088/0004-637X/759/1/71
Usage Policy:No commercial reproduction, distribution, display or performance rights in this work are provided.
ID Code:36021
Collection:CaltechAUTHORS
Deposited By: Ruth Sustaita
Deposited On:18 Dec 2012 16:42
Last Modified:09 Mar 2020 13:19

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