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Titolo:
Observation and modeling of the solar transition region. I. Multi-spectralsolar telescope array observations
Autore:
Oluseyi, HM; Walker, ABC; Porter, J; Hoover, RB; Barbee, TW;
Indirizzi:
Stanford Univ, Dept Phys, Stanford, CA 94305 USA Stanford Univ Stanford CA USA 94305 iv, Dept Phys, Stanford, CA 94305 USA Stanford Univ, Ctr Space Sci & Astrophys, Stanford, CA 94305 USA Stanford Univ Stanford CA USA 94305 i & Astrophys, Stanford, CA 94305 USA Stanford Univ, Dept Appl Phys, Stanford, CA 94305 USA Stanford Univ Stanford CA USA 94305 ept Appl Phys, Stanford, CA 94305 USA NASA, George C Marshall Space Flight Ctr, Space Sci Lab, Huntsville, AL 35812 USA NASA Huntsville AL USA 35812 Ctr, Space Sci Lab, Huntsville, AL 35812 USA Univ Calif Lawrence Livermore Natl Lab, Dept Chem & Mat Sci, Livermore, CA94550 USA Univ Calif Lawrence Livermore Natl Lab Livermore CA USA 94550 CA94550 USA
Titolo Testata:
ASTROPHYSICAL JOURNAL
fascicolo: 2, volume: 524, anno: 1999,
parte:, 1
pagine: 1105 - 1121
SICI:
0004-637X(19991020)524:2<1105:OAMOTS>2.0.ZU;2-9
Fonte:
ISI
Lingua:
ENG
Soggetto:
UNRESOLVED FINE-STRUCTURES; RAY BRIGHT POINTS; ENERGY-BALANCE; CORONAL LOOPS; POLAR PLUMES; QUIET SUN; TEMPERATURE REGION; MAGNETIC-STRUCTURE; ACTIVE REGIONS; SCALING LAW;
Keywords:
Sun : chromosphere; Sun : transition region; Sun : UV radiation;
Tipo documento:
Article
Natura:
Periodico
Settore Disciplinare:
Physical, Chemical & Earth Sciences
Citazioni:
89
Recensione:
Indirizzi per estratti:
Indirizzo: Oluseyi, HM Stanford Univ, Dept Phys, Stanford, CA 94305 USA Stanford Univ Stanford CA USA 94305 s, Stanford, CA 94305 USA
Citazione:
H.M. Oluseyi et al., "Observation and modeling of the solar transition region. I. Multi-spectralsolar telescope array observations", ASTROPHYS J, 524(2), 1999, pp. 1105-1121

Abstract

We report on observations of the solar atmosphere in several extreme-ultraviolet and far-ultraviolet bandpasses obtained by the Multi-Spectral Solar Telescope Array, a rocket-borne spectroheliograph, on flights in 1987, 1991, and 1994, spanning the last solar maximum. Quiet-Sun emission observed inthe 171-175 Angstrom bandpass, which includes lines of O V, O VI, Fe rx, and Fe X, has been analyzed to test models of the temperatures and geometries of the structures responsible for this emission. Analyses of intensity variations above the solar limb reveal scale heights consistent with a quiet-Sun plasma temperature of 500,000 less than or equal to T-e less than or equal to 800,000 K. The structures responsible for the quiet-Sun EUV emissionare modeled as small quasi-static loops. We submit our models to several tests. We compare the emission our models would produce in the bandpass of our telescope to the emission we have observed. We find that the emission predicted by loop models with maximum temperatures between 700,000 and 900,000 K are consistent with our observations. We also compare the absolute fluxpredicted by our models in a typical upper transition region line to the flux measured by previous observers. Finally, we present a preliminary comparison of the predictions of our models with diagnostic spectral line ratiosfrom previous observers. Intensity modulations in the quiet Sun are observed to occur on a scale comparable to the supergranular scale. We discuss the implications that a distribution of loops of the type we model here wouldhave for heating the local network at the loops' footpoints.

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Documento generato il 13/07/20 alle ore 07:45:32