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Statements

Subject Item
n2:RIV%2F00216305%3A26210%2F10%3APU88267%21RIV11-GA0-26210___
rdf:type
n4:Vysledek skos:Concept
dcterms:description
The structure of the white-light and emission solar coronas and their MHD modelling are the context of our work. . A comparison is made between the structure of the solar corona as observed during the 2008 August 1 total eclipse from Mongolia and that predicted by an MHD model. The model has an improved energy formulation, including the effect of coronal heating, conduction of heat parallel to the magnetic field, radiative losses, and acceleration by Alfvén waves. The white-light corona, which was visible up to 20 solar radii, was of an intermediate type with well-pronounced helmet streamers situated above a chain of prominences at position angles of 48, 130, 241, and 322 degrees. Two polar coronal holes, filled with a plethora of thin polar plumes, were observed. High-quality pictures of the green (530.3 nm, Fe XIV) corona were obtained with the help of two narrow-passband filters (centered at the line itself and the vicinity of 529.1 nm background), with a FWHM of 0.15 nm. The large-scale shape of The structure of the white-light and emission solar coronas and their MHD modelling are the context of our work. . A comparison is made between the structure of the solar corona as observed during the 2008 August 1 total eclipse from Mongolia and that predicted by an MHD model. The model has an improved energy formulation, including the effect of coronal heating, conduction of heat parallel to the magnetic field, radiative losses, and acceleration by Alfvén waves. The white-light corona, which was visible up to 20 solar radii, was of an intermediate type with well-pronounced helmet streamers situated above a chain of prominences at position angles of 48, 130, 241, and 322 degrees. Two polar coronal holes, filled with a plethora of thin polar plumes, were observed. High-quality pictures of the green (530.3 nm, Fe XIV) corona were obtained with the help of two narrow-passband filters (centered at the line itself and the vicinity of 529.1 nm background), with a FWHM of 0.15 nm. The large-scale shape of The structure of the white-light and emission solar coronas and their MHD modelling are the context of our work. . A comparison is made between the structure of the solar corona as observed during the 2008 August 1 total eclipse from Mongolia and that predicted by an MHD model. The model has an improved energy formulation, including the effect of coronal heating, conduction of heat parallel to the magnetic field, radiative losses, and acceleration by Alfvén waves. The white-light corona, which was visible up to 20 solar radii, was of an intermediate type with well-pronounced helmet streamers situated above a chain of prominences at position angles of 48, 130, 241, and 322 degrees. Two polar coronal holes, filled with a plethora of thin polar plumes, were observed. High-quality pictures of the green (530.3 nm, Fe XIV) corona were obtained with the help of two narrow-passband filters (centered at the line itself and the vicinity of 529.1 nm background), with a FWHM of 0.15 nm. The large-scale shape of
dcterms:title
Comparing eclipse observations of the 2008 August 1 solar corona with an MHD model prediction Comparing eclipse observations of the 2008 August 1 solar corona with an MHD model prediction Comparing eclipse observations of the 2008 August 1 solar corona with an MHD model prediction
skos:prefLabel
Comparing eclipse observations of the 2008 August 1 solar corona with an MHD model prediction Comparing eclipse observations of the 2008 August 1 solar corona with an MHD model prediction Comparing eclipse observations of the 2008 August 1 solar corona with an MHD model prediction
skos:notation
RIV/00216305:26210/10:PU88267!RIV11-GA0-26210___
n3:aktivita
n13:P
n3:aktivity
P(GA205/09/1469)
n3:cisloPeriodika
5
n3:dodaniDat
n14:2011
n3:domaciTvurceVysledku
n18:8961905
n3:druhVysledku
n11:J
n3:duvernostUdaju
n9:S
n3:entitaPredkladatele
n6:predkladatel
n3:idSjednocenehoVysledku
251348
n3:idVysledku
RIV/00216305:26210/10:PU88267
n3:jazykVysledku
n16:cze
n3:klicovaSlova
sun, corona, magnetic field, MHD model
n3:klicoveSlovo
n10:MHD%20model n10:corona n10:sun n10:magnetic%20field
n3:kodStatuVydavatele
FR - Francouzská republika
n3:kontrolniKodProRIV
[A35F0C353C15]
n3:nazevZdroje
ASTRONOMY & ASTROPHYSICS
n3:obor
n15:BN
n3:pocetDomacichTvurcuVysledku
1
n3:pocetTvurcuVysledku
10
n3:projekt
n17:GA205%2F09%2F1469
n3:rokUplatneniVysledku
n14:2010
n3:svazekPeriodika
2010 (513)
n3:tvurceVysledku
Rušin, Vojtěch Linker, J. A Riley, P. Aniol, Peter Lionello, R. Mikič, Zoran Druckmüller, Miloslav Minarovjech, Milan Titov, V. S. Saniga, Metod
s:issn
0004-6361
s:numberOfPages
7
n7:organizacniJednotka
26210