%0 Journal Article
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%@nexthigherunit 8JMKD3MGPCW/3ETR8EH
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%@resumeid 8JMKD3MGP5W/3C9JH2C
%X This article broadly reviews our knowledge of solar flares. There is a particular focus on their global properties, as opposed to the microphysics such as that needed for magnetic reconnection or particle acceleration as such. Indeed solar flares will always remain in the domain of remote sensing, so we cannot observe the microscales directly and must understand the basic physics entirely via the global properties plus theoretical inference. The global observables include the general energeticsradiation in flares and mass loss in coronal mass ejections (CMEs)and the formation of different kinds of ejection and global wave disturbance: the type II radio-burst exciter, the Moreton wave, the EIT wave, and the sunquake acoustic waves in the solar interior. Flare radiation and CME kinetic energy can have comparable magnitudes, of order 1032 erg each for an X-class event, with the bulk of the radiant energy in the visible-UV continuum. We argue that the impulsive phase of the flare dominates the energetics of all of these manifestations, and also point out that energy and momentum in this phase largely reside in the electromagnetic field, not in the observable plasma.
%N 2
%T Unusual emissions at various energies prior to the impulsive phase of the large solar flare and coronal mass ejection of 4 november 2003
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%@electronicmailaddress ecorreia@craam.mackenzie.br
%@secondarytype PRE PI
%K solar flares, CME, submillimeter emission, RHESSI X-ray emissions.
%@archivingpolicy denypublisher denyfinaldraft12
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%@usergroup banon
%@usergroup lattes
%@usergroup secretaria.cpa@dir.inpe.br
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%@group DAS-CEA-INPE-MCTI-GOV-BR
%@e-mailaddress ecorreia@craam.mackenzie.br
%3 Kaufmann-SolPhys-fulltext[1].pdf
%@secondarykey INPE--PRE/
%@secondarymark B1_ASTRONOMIA_/_FÍSICA B1_BIOTECNOLOGIA B2_CIÊNCIA_DA_COMPUTAÇÃO B1_ENGENHARIAS_IV A1_GEOCIÊNCIAS A2_INTERDISCIPLINAR
%F lattes: 1272123236892781 5 KaufmannHSGCFSMP:2012:UnEmVa
%@issn 0038-0938
%@issn 1573-093X
%2 dpi.inpe.br/plutao/2012/06.21.18.39.30
%@affiliation Escola de Engenharia, CRAAM, Universidade Presbiteriana Mackenzie, São Paulo, SP 01302970
%@affiliation ·National Aeronautics and Space Administration, Goddard Space Flight Center, Code 671, Greenbelt
%@affiliation Department of Physics, The Catholic University of America, Washington, DC 20064, USA
%@affiliation CRAAM, Universidade Presbiteriana Mackenzie, São Paulo, SP 01302970
%@affiliation Instituto Nacional de Pesquisas Espaciais (INPE)
%@affiliation Escola de Engenharia, CRAAM, Universidade Presbiteriana Mackenzie, São Paulo, SP 01302970
%@affiliation Escola de Engenharia, CRAAM, Universidade Presbiteriana Mackenzie, São Paulo, SP 01302970
%@affiliation Complejo Astronômico El Leoncito, CONICET, San Juan, Argentina
%@affiliation ·Complejo Astronômico El Leoncito, CONICET, San Juan, Argentina
%B Solar Physics
%@versiontype publisher
%P 465-475
%4 dpi.inpe.br/plutao/2012/06.21.18.39
%@documentstage not transferred
%D 2012
%V 279
%@doi 10.1007/s11207-012-0040-7
%A Kaufmann, P.,
%A Holman, G. D.,
%A Su, Y.,
%A Giménez de Castro, C. G.,
%A Correia, Emilia,
%A Fernandes, L. O. T.,
%A Souza, Rodney V de,
%A Marun, A.,
%A Pereyra, P.,
%@dissemination WEBSCI; PORTALCAPES.
%@area CEA