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Titolo: Centimetric type N and type M bursts
Autore: Wang, M; Fu, Q; Xie, R; Duan, C;
- Indirizzi:
- Chinese Acad Sci, Yunnan Observ, Natl Astron Observ, Kunming 650011, Peoples R China Chinese Acad Sci Kunming Peoples R China 650011 650011, Peoples R China Chinese Acad Sci, Natl Astron Observ, Beijing 100012, Peoples R China Chinese Acad Sci Beijing Peoples R China 100012 100012, Peoples R China
- Titolo Testata:
- ASTRONOMY & ASTROPHYSICS
fascicolo: 1,
volume: 380,
anno: 2001,
pagine: 318 - 322
- SICI:
- 1432-0746(200112)380:1<318:CTNATM>2.0.ZU;2-1
- Fonte:
- ISI
- Lingua:
- ENG
- Soggetto:
- SOLAR RADIO-BURSTS; CORONAL LOOPS; ELECTRONS; FLARES; BEAMS;
- Keywords:
- Sun : activity; Sun : corona; Sun : general; Sun : radio radiation;
- Tipo documento:
- Article
- Natura:
- Periodico
- Settore Disciplinare:
- Physical, Chemical & Earth Sciences
- Citazioni:
- 18
- Recensione:
- Indirizzi per estratti:
- Indirizzo: Wang, M Chinese Acad Sci, Yunnan Observ, Natl Astron Observ, Kunming 650011, Peoples R China Chinese Acad Sci Kunming Peoples R China 650011 Peoples R China
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- Citazione:
- M. Wang et al., "Centimetric type N and type M bursts", ASTRON ASTR, 380(1), 2001, pp. 318-322
Abstract
Two special fine structures observed with the 5.2-7.6 GHz high temporal and spectral resolution spectrometer of Beijing Astronomical Observatory (BAO) are described and analyzed in this paper. Because they appear as the letters N and M on dynamic spectra, we call them centimetric type N and type M bursts, respectively. They have very short durations (about 500 ms and 300 ms), small flux densities (tens of SFU), narrow bandwidth (relative bandwidth about 10%), and very small polarization degree (close to the accuracy limit of observation instruments), but each branch has considerable high frequency drift rates (several GHz/s). We think that they are an extension of metric or decimetric type U(N) bursts in centimetric wavelengths. Type N andtype M bursts may be due to the mirroring effect near the foot point, as well as a scattering effect caused by whistler wave turbulence near the top of loop. They may also be interpreted by the quasi-periodic particle injection into coronal loops.
ASDD Area Sistemi Dipartimentali e Documentali, Università di Bologna, Catalogo delle riviste ed altri periodici
Documento generato il 20/06/13 alle ore 08:56:05