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Titolo:
EUV SPECTROSCOPY OF THE SUNSPOT REGION NOAA-7981 USING SOHO I - LINE EMISSION AND TUNE DEPENDENCE
Autore:
BRYNILDSEN N; BREKKE P; FREDVIK T; HAUGAN SVH; KJELDSETHMOE O; MALTBY P; HARRISON RA; PIKE CD; RIMMELE T; THOMPSON WT; WILHELM K;
Indirizzi:
UNIV OSLO,INST THEORET ASTROPHYS N-0315 OSLO NORWAY RUTHERFORD APPLETON LAB,DEPT SPACE SCI DIDCOT OX11 0QX OXON ENGLAND NATL SOLAR OBSERV SUNSPOT NM 88349 APPL RES CORP LANDOVER MD 20785 MAX PLANCK INST AERON D-37191 KATLENBURG DUHM GERMANY
Titolo Testata:
Solar physics
fascicolo: 1, volume: 179, anno: 1998,
pagine: 43 - 74
SICI:
0038-0938(1998)179:1<43:ESOTSR>2.0.ZU;2-I
Fonte:
ISI
Lingua:
ENG
Soggetto:
CORONA TRANSITION REGION; ULTRAVIOLET-SPECTRUM; TEMPORAL VARIATIONS; FLUID MOTIONS; SOLAR; PRESSURE; BALANCE; PLUMES; LOOPS;
Tipo documento:
Article
Natura:
Periodico
Settore Disciplinare:
Science Citation Index Expanded
Citazioni:
48
Recensione:
Indirizzi per estratti:
Citazione:
N. Brynildsen et al., "EUV SPECTROSCOPY OF THE SUNSPOT REGION NOAA-7981 USING SOHO I - LINE EMISSION AND TUNE DEPENDENCE", Solar physics, 179(1), 1998, pp. 43-74

Abstract

EUV spectra of a medium-size sunspot and its surroundings, NOAA 7981,were obtained on 2 August 1996 with the Coronal Diagnostic Spectrometer (CDS) and the Solar Ultraviolet Measurements of Emitted Radiation (SUMER) on the Solar and Heliospheric Observatory (SOHO). The spectral lines formed in the transition region and corona show considerable structure and large deviations from a uniform spatial distribution over the active region. Enhanced EUV emissions in transition region lines are concentrated in small regions outside the umbra of the sunspot throughout most of the observing sequence. Only during a short, active period do we find an enhanced line emission that reaches into the umbra. Preliminary values for the umbral intensity are given. Marked changes are detected between the spatial distribution of line emission in the transition region and the low corona. The difference is not limited to cool and hot non-flaring loops not being cospatial, but includes differences both regarding the time variability and the orientation and size of the emission features. Whereas both rapid (approximate to 4 and 2min) and slow (approximate to 10 and 12 h) temporal variations are found in the chromosphere (He I 584 Angstrom) and transition region (O V629 Angstrom), the response in the low corona (Mg IX 368 Angstrom) isslow (approximate to 5 h). Furthermore, marked differences between the spatial distributions in the Mg VIII 315 Angstrom, Mg IX 368 Angstrom lines formed in the low corona and the coronal Fe XIV 334 Angstrom, Fe XVI 360 Angstrom lines are detected.

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Documento generato il 26/09/20 alle ore 22:49:07