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dc.contributor.CRUESPUniversidade Estadual de Campinaspt_BR
dc.typeArtigo de periódicopt_BR
dc.titleA new solar burst spectral component emitting only in the terahertz rangept_BR
dc.contributor.authorKaufmann, Ppt_BR
dc.contributor.authorRaulin, JPpt_BR
dc.contributor.authorde Castro, CGGpt_BR
dc.contributor.authorLevato, Hpt_BR
dc.contributor.authorGary, DEpt_BR
dc.contributor.authorCosta, JERpt_BR
dc.contributor.authorMarun, Apt_BR
dc.contributor.authorPereyra, Ppt_BR
dc.contributor.authorSilva, AVRpt_BR
dc.contributor.authorCorreia, Ept_BR
unicamp.authorUniv Presbiteriana Mackenzie, CRAAM, BR-01302907 Sao Paulo, Brazil Univ Estadual Campinas, Ctr Componentes Semicond, BR-01398397 Campinas, SP, Brazil CASLEO, RA-5400 San Juan, Argentina New Jersey Inst Technol, Owens Valley Solar Array, Newark, NJ 07102 USA INPE, BR-12227010 Sao Jose Dos Campos, Brazilpt_BR
dc.subjectplasmaspt_BR
dc.subjectradiation mechanisms : nonthermalpt_BR
dc.subjectsubmillimeterpt_BR
dc.subjectSun : flarespt_BR
dc.subjectSun : infraredpt_BR
dc.subjectSun : radio radiationpt_BR
dc.subject.wosX-rayspt_BR
dc.subject.wosFlarespt_BR
dc.subject.wosFrequencypt_BR
dc.subject.wosContinuumpt_BR
dc.subject.wosRadiationpt_BR
dc.subject.wosTimept_BR
dc.subject.wosHardpt_BR
dc.description.abstractSolar flare energy manifestations were believed to be the result of the same kind of particle acceleration. It is generally accepted that a population of relativistic electrons accelerated during the impulsive phase of solar flares produces microwaves by synchrotron losses in the solar magnetic field and X-rays by collisions in denser regions of the solar atmosphere. We report the discovery of a new intense solar flare spectral radiation component, peaking somewhere in the shorter submillimeter to far-infrared range, identified during the 2003 November 4 large flare. The new solar submillimeter telescope, designed to extend the frequency range to above 100 GHz, detected this new component with increasing fluxes between 212 and 405 GHz. It appears along with, but is separated from, the well-known gyrosynchrotron emission component seen at microwave frequencies. The novel emission component had three major peaks with time, originated in a compact source whose position remained remarkably steady within 15'. Intense subsecond pulses are superposed with excess fluxes also increasing with frequency and amplitude increasing with the pulse repetition rate. The origin of the terahertz emission component during the flare impulsive phase is not known. It might be representative of emission due to electrons with energies considerably larger than the energies assumed to explain emission at microwaves. This component can attain considerably larger intensities in the far-infrared, with a spectrum extending to the white-light emission observed for that flare.pt
dc.relation.ispartofAstrophysical Journalpt_BR
dc.relation.ispartofabbreviationAstrophys. J.pt_BR
dc.publisher.cityChicagopt_BR
dc.publisher.countryEUApt_BR
dc.publisherUniv Chicago Presspt_BR
dc.date.issued2004pt_BR
dc.date.monthofcirculation40238pt_BR
dc.identifier.citationAstrophysical Journal. Univ Chicago Press, v. 603, n. 2, n. L121, n. L124, 2004.pt_BR
dc.language.isoenpt_BR
dc.description.volume603pt_BR
dc.description.issuenumber2pt_BR
dc.description.issuepart2pt_BR
dc.description.firstpageL121pt_BR
dc.description.lastpageL124pt_BR
dc.rightsabertopt_BR
dc.sourceWeb of Sciencept_BR
dc.identifier.issn0004-637Xpt_BR
dc.identifier.wosidWOS:000220300800015pt_BR
dc.identifier.doi10.1086/383186pt_BR
dc.date.available2014-11-14T04:03:25Z
dc.date.available2015-11-26T16:04:20Z-
dc.date.accessioned2014-11-14T04:03:25Z
dc.date.accessioned2015-11-26T16:04:20Z-
dc.description.provenanceMade available in DSpace on 2014-11-14T04:03:25Z (GMT). No. of bitstreams: 1 WOS000220300800015.pdf: 131127 bytes, checksum: add983699ba993ab4bd8a88615042d36 (MD5) Previous issue date: 2004en
dc.description.provenanceMade available in DSpace on 2015-11-26T16:04:20Z (GMT). No. of bitstreams: 2 WOS000220300800015.pdf: 131127 bytes, checksum: add983699ba993ab4bd8a88615042d36 (MD5) WOS000220300800015.pdf.txt: 18693 bytes, checksum: b0548a197ed0d7087a257d9e89a87ceb (MD5) Previous issue date: 2004en
dc.identifier.urihttp://www.repositorio.unicamp.br/jspui/handle/REPOSIP/76345pt_BR
dc.identifier.urihttp://www.repositorio.unicamp.br/handle/REPOSIP/76345
dc.identifier.urihttp://repositorio.unicamp.br/jspui/handle/REPOSIP/76345-
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