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Titolo: Nonthermal flare emission from MeV-energy electrons at 17, 34, and 86 GHz
Autore: Kundu, MR; White, SM; Shibasaki, K; Sakurai, T;
- Indirizzi:
- Univ Maryland, Dept Astron, College Pk, MD 20742 USA Univ Maryland College Pk MD USA 20742 pt Astron, College Pk, MD 20742 USA Natl Astron Observ, Nobeyama Radio Observ, Minamisa Ku, Nagano 38413, Japan Natl Astron Observ Nagano Japan 38413 , Minamisa Ku, Nagano 38413, Japan Natl Astron Observ, Mitaka, Tokyo 1818588, Japan Natl Astron Observ Mitaka Tokyo Japan 1818588 itaka, Tokyo 1818588, Japan
- Titolo Testata:
- ASTROPHYSICAL JOURNAL
fascicolo: 2,
volume: 545,
anno: 2000,
parte:, 1
pagine: 1084 - 1088
- SICI:
- 0004-637X(200012)545:2<1084:NFEFME>2.0.ZU;2-#
- Fonte:
- ISI
- Lingua:
- ENG
- Soggetto:
- SOFT-X-RAY; SOLAR-FLARES; RADIO-EMISSION; MICROWAVE; MILLIMETER; LOOP;
- Keywords:
- Sun : corona; Sun : flares; Sun : radio radiation;
- Tipo documento:
- Article
- Natura:
- Periodico
- Settore Disciplinare:
- Physical, Chemical & Earth Sciences
- Citazioni:
- 15
- Recensione:
- Indirizzi per estratti:
- Indirizzo: Kundu, MR Univ Maryland, Dept Astron, College Pk, MD 20742 USA Univ Maryland College Pk MD USA 20742 College Pk, MD 20742 USA
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- Citazione:
- M.R. Kundu et al., "Nonthermal flare emission from MeV-energy electrons at 17, 34, and 86 GHz", ASTROPHYS J, 545(2), 2000, pp. 1084-1088
Abstract
We present analyses of two solar flares observed with high spatial resolution at 86 GHz with the BIMA millimeter-wavelength telescope and at 17 and 34 GHz with the Nobeyama radioheliograph. The flares were observed on 1998 November 24 and 1999 May 1. At millimeter wavelengths these are impulsive events, and therefore they must be produced by MeV-energy electrons. The present study using simultaneous observations of two flares at 86, 34, and 17 GHz provides an excellent opportunity to study high-energy electrons with high spatial resolution observations at three optically thin frequencies. Themorphology of millimeter emission can reveal both the properties of the MeV-energy electrons and the nature of the coronal magnetic field lines wherethey radiate. One of the two events we present is the first clear case of a lambda = 3 mm source in which both footpoints of a loop are detected. In the second event the polarization image at 17 GHz also suggests a bipolar or looplike morphology. Such morphological observations can be used to constrain the nature of the magnetic field in the solar corona.
ASDD Area Sistemi Dipartimentali e Documentali, Università di Bologna, Catalogo delle riviste ed altri periodici
Documento generato il 26/05/13 alle ore 04:35:02