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Statements

Subject Item
n2:RIV%2F00216305%3A26210%2F07%3APU66110%21RIV07-MSM-26210___
rdf:type
n5:Vysledek skos:Concept
dcterms:description
Solar eclipse observations have long suggested that the white-light corona is permeated by long fine rays. By comparing photographs of the 2006 March 29 total eclipse with current-free extrapolations of photospheric field measurements and with images from the Solar and Heliospheric Observatory (SOHO), we deduce that the bulk of these linear features fall into three categories: (1) polar and low-latitude plumes that overlie small magnetic bipoles inside coronal holes, (2) helmet streamer rays that overlie large loop arcades and separate coronal holes of opposite polarity, and (3) %22pseudostreamer%22 rays that overlie twin loop arcades and separate coronal holes of the same polarity. The helmet streamer rays extend outward to form the plasma sheet component of the slow solar wind, while the plumes and pseudostreamers contribute to the fast solar wind. In all three cases, the rays are formed by magnetic reconnection between closed coronal loops and adjacent open field lines. Although seemingly ubiquitous wh Solar eclipse observations have long suggested that the white-light corona is permeated by long fine rays. By comparing photographs of the 2006 March 29 total eclipse with current-free extrapolations of photospheric field measurements and with images from the Solar and Heliospheric Observatory (SOHO), we deduce that the bulk of these linear features fall into three categories: (1) polar and low-latitude plumes that overlie small magnetic bipoles inside coronal holes, (2) helmet streamer rays that overlie large loop arcades and separate coronal holes of opposite polarity, and (3) %22pseudostreamer%22 rays that overlie twin loop arcades and separate coronal holes of the same polarity. The helmet streamer rays extend outward to form the plasma sheet component of the slow solar wind, while the plumes and pseudostreamers contribute to the fast solar wind. In all three cases, the rays are formed by magnetic reconnection between closed coronal loops and adjacent open field lines. Although seemingly ubiquitous wh Solar eclipse observations have long suggested that the white-light corona is permeated by long fine rays. By comparing photographs of the 2006 March 29 total eclipse with current-free extrapolations of photospheric field measurements and with images from the Solar and Heliospheric Observatory (SOHO), we deduce that the bulk of these linear features fall into three categories: (1) polar and low-latitude plumes that overlie small magnetic bipoles inside coronal holes, (2) helmet streamer rays that overlie large loop arcades and separate coronal holes of opposite polarity, and (3) %22pseudostreamer%22 rays that overlie twin loop arcades and separate coronal holes of the same polarity. The helmet streamer rays extend outward to form the plasma sheet component of the slow solar wind, while the plumes and pseudostreamers contribute to the fast solar wind. In all three cases, the rays are formed by magnetic reconnection between closed coronal loops and adjacent open field lines. Although seemingly ubiquitous wh
dcterms:title
The Solar Eclipse of 2006 and the Origin of Raylike Features in the White-Light Corona The Solar Eclipse of 2006 and the Origin of Raylike Features in the White-Light Corona The Solar Eclipse of 2006 and the Origin of Raylike Features in the White-Light Corona
skos:prefLabel
The Solar Eclipse of 2006 and the Origin of Raylike Features in the White-Light Corona The Solar Eclipse of 2006 and the Origin of Raylike Features in the White-Light Corona The Solar Eclipse of 2006 and the Origin of Raylike Features in the White-Light Corona
skos:notation
RIV/00216305:26210/07:PU66110!RIV07-MSM-26210___
n3:strany
882-892
n3:aktivita
n11:S
n3:aktivity
S
n3:cisloPeriodika
3
n3:dodaniDat
n17:2007
n3:domaciTvurceVysledku
n10:8961905
n3:druhVysledku
n9:J
n3:duvernostUdaju
n16:S
n3:entitaPredkladatele
n15:predkladatel
n3:idSjednocenehoVysledku
450909
n3:idVysledku
RIV/00216305:26210/07:PU66110
n3:jazykVysledku
n6:eng
n3:klicovaSlova
solar streemer
n3:klicoveSlovo
n13:solar%20streemer
n3:kodStatuVydavatele
US - Spojené státy americké
n3:kontrolniKodProRIV
[865E2860DE3A]
n3:nazevZdroje
ASTROPHYSICAL JOURNAL
n3:obor
n12:BL
n3:pocetDomacichTvurcuVysledku
1
n3:pocetTvurcuVysledku
6
n3:rokUplatneniVysledku
n17:2007
n3:svazekPeriodika
660
n3:tvurceVysledku
Mouette, J. Sheeley, N. R. Koutchmy, Serge Druckmüller, Miloslav Biersteker, T. J. Wang, Y. M.
s:issn
0004-637X
s:numberOfPages
11
n7:organizacniJednotka
26210