Pregled bibliografske jedinice broj: 1265291
EUV brightness variations in the quiet Sun
EUV brightness variations in the quiet Sun // Astronomy & Astrophysics, 353 (2000), 1083-1093 (međunarodna recenzija, članak, znanstveni)
CROSBI ID: 1265291 Za ispravke kontaktirajte CROSBI podršku putem web obrasca
Naslov
EUV brightness variations in the quiet Sun
Autori
Brković, Alen, Rüedi, Isabelle, Solanki, Sami Khan, Fludra, Andrzej, Harrison, Richard Anthony, Huber, Martin Christoph Emanuele, Stenflo, Jan Olof, Stucki, Katja
Izvornik
Astronomy & Astrophysics (0004-6361) 353
(2000);
1083-1093
Vrsta, podvrsta i kategorija rada
Radovi u časopisima, članak, znanstveni
Ključne riječi
Sun: chromosphere -- Sun: corona -- Sun: transition region -- Sun: UV radiation
Sažetak
The Coronal Diagnostic Spectrometer (CDS) onboard the SOHO satellite has been used to obtain movies of quiet Sun regions at disc centre. These movies were used to study brightness variations of solar features at three different temperatures sampled simultaneously in the chromospheric He I 584.3 Å (20 000 K), the transition region O V 629.7 Å (250 000 K) and coronal Mg IX 368.1 Å (1 000 000 K) lines. In all parts of the quiet Sun, from darkest intranetwork to brightest network, we find significant variability in the He I and O V line, while the variability in the Mg IX line is more marginal. The relative variability, defined by rms of intensity normalised to the local intensity, is independent of brightness and strongest in the transition region line. Thus the relative variability is the same in the network and the intranetwork. More than half of the points on the solar surface show a relative variability, determined over a period of 4 hours, greater than 15.5 % for the O V line, but only 5 % of the points exhibit a variability above 25 %. Most of the variability appears to take place on time-scales between 5 and 80 minutes for the He I and O V lines. Clear signs of ``high variability'' events are found. For these events the variability as a function of time seen in the different lines shows a good correlation. The correlation is higher for more variable events. These events coincide with the (time averaged) brightest points on the solar surface, i.e. they occur in the network. The spatial positions of the most variable points are identical in all the lines.
Izvorni jezik
Engleski
Znanstvena područja
Fizika
POVEZANOST RADA
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Časopis indeksira:
- Current Contents Connect (CCC)
- Web of Science Core Collection (WoSCC)
- Science Citation Index Expanded (SCI-EXP)
- SCI-EXP, SSCI i/ili A&HCI
- Scopus