http://www.cnr.it/ontology/cnr/individuo/prodotto/ID1400

Electron-electron bremsstrahlung emission and the inference of electron flux spectra in solar flares (Articolo in rivista)

Type

Articolo in rivista (Classe)
Prodotto della ricerca (Classe)

Label

Electron-electron bremsstrahlung emission and the inference of electron flux spectra in solar flares (Articolo in rivista) (literal)

Anno

2007-01-01T00:00:00+01:00 (literal)

Alternative label

Kontar, EP; Emslie, AG; Massone, AM; Piana, M; Brown, JC; Prato, M (2007)
Electron-electron bremsstrahlung emission and the inference of electron flux spectra in solar flares
in Astrophysical journal (Online)
(literal)

Http://www.cnr.it/ontology/cnr/pubblicazioni.owl#autori

Kontar, EP; Emslie, AG; Massone, AM; Piana, M; Brown, JC; Prato, M (literal)

Pagina inizio

857 (literal)

Pagina fine

861 (literal)

Http://www.cnr.it/ontology/cnr/pubblicazioni.owl#numeroVolume

670 (literal)

Rivista

Astrophysical journal (Rivista)

Note

Google Scholar (literal)
ISI Web of Science (WOS) (literal)
Scopus (literal)

Http://www.cnr.it/ontology/cnr/pubblicazioni.owl#affiliazioni

Univ Glasgow, Dept Phys, Glasgow G12 8QQ, Lanark, Scotland; Oklahoma State Univ, Dept Phys, Stillwater, OK 74078 USA; INFM, CNR, LAMIA, I-16146 Genoa, Italy; Univ Verona, Dipartimento Informat, I-37134 Verona, Italy; Univ Modena, Dipartimento Matemat, I-41100 Modena, Italy (literal)

Titolo

Electron-electron bremsstrahlung emission and the inference of electron flux spectra in solar flares (literal)

Abstract

Although both electron-ion and electron-electron bremsstrahlung contribute to the hard X-ray emission from solar flares, the latter is normally ignored. Such anomission is not justified at electron (and photon) energies above?300 keV, and inclusion of the additional electron-electron bremsstrahlung in general makes the electron spectrum required to produce a given hard X-ray spectrum steeper at high energies. Unlike electron-ion bremsstrahlung, electron-electron bremsstrahlung cannot produce photons of all energies up to the electron energy involved. Themaximum possible photon energy depends on the angle between the direction of the emitting electron and the emitted photon, and this suggests a diagnostic for an upper cutoff energy and/or for the degree of beaming of the accelerated electrons. We analyze the large event of 2005 January 17 and show that the upward break around 400 keVin the observed hard X-ray spectrum is naturally accounted for by the inclusion of electron-electron bremsstrahlung. Indeed, the mean source electron spectrum recovered through a regularized inversion of the hard X-ray spectrum, using a cross section that includes both electronion and electron-electron terms, has a relatively constant spectral index ? over the range from electron kinetic energy E = 200 keV to E = 1 MeV. Such a spectrum is indicative of an acceleration mechanism without a characteristic energy or corresponding scale. (literal)
Although both electron-ion and electron-electron bremsstrahlung contribute to the hard X-ray emission from solar flares, the latter is normally ignored. Such an omission is not justified at electron (and photon) energies above similar to 300 keV, and inclusion of the additional electron-electron bremsstrahlung in general makes the electron spectrum required to produce a given hard X-ray spectrum steeper at high energies. Unlike electron-ion bremsstrahlung, electron-electron bremsstrahlung cannot produce photons of all energies up to the electron energy involved. The maximum possible photon energy depends on the angle between the direction of the emitting electron and the emitted photon, and this suggests a diagnostic for an upper cutoff energy and/ or for the degree of beaming of the accelerated electrons. We analyze the large event of 2005 January 17 and show that the upward break around 400 keV in the observed hard X-ray spectrum is naturally accounted for by the inclusion of electron-electron bremsstrahlung. Indeed, the mean source electron spectrum recovered through a regularized inversion of the hard X-ray spectrum, using a cross section that includes both electronion and electron-electron terms, has a relatively constant spectral index delta over the range from electron kinetic energy E = 200 keV to E = 1 MeV. Such a spectrum is indicative of an acceleration mechanism without a characteristic energy or corresponding scale. (literal)

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