Detail publikace
Comparing eclipse observations of the 2008 August 1 solar corona with an MHD model prediction
RUŠIN, V. DRUCKMÜLLER, M. ANIOL, P. MINAROVJECH, M. SANIGA, M. MIKIČ, Z. LINKER, J. LIONELLO, R. RILEY, P. TITOV, V.
Český název
Comparing eclipse observations of the 2008 August 1 solar corona with an MHD model prediction
Anglický název
Comparing eclipse observations of the 2008 August 1 solar corona with an MHD model prediction
Typ
článek v časopise - ostatní, Jost
Jazyk
cs
Originální abstrakt
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 both the white-light and green corona was found to agree well with that predicted by the model. In this paper we describe the morphological properties of the observed corona, and how it compares with that predicted by the model.
Český abstrakt
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 both the white-light and green corona was found to agree well with that predicted by the model. In this paper we describe the morphological properties of the observed corona, and how it compares with that predicted by the model.
Anglický abstrakt
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 both the white-light and green corona was found to agree well with that predicted by the model. In this paper we describe the morphological properties of the observed corona, and how it compares with that predicted by the model.
Klíčová slova česky
sun, corona, magnetic field, MHD model
Klíčová slova anglicky
sun, corona, magnetic field, MHD model
Rok RIV
2010
Vydáno
10.02.2010
ISSN
0004-6361
Časopis
ASTRONOMY & ASTROPHYSICS
Ročník
2010 (513)
Číslo
5
Strany od–do
49–56
Počet stran
7
BIBTEX
@article{BUT50772,
author="Vojtěch {Rušin} and Miloslav {Druckmüller} and Peter {Aniol} and Milan {Minarovjech} and Metod {Saniga} and Zoran {Mikič} and J.A. {Linker} and R. {Lionello} and P. {Riley} and V.S. {Titov},
title="Comparing eclipse observations of the 2008 August 1 solar corona with an MHD model prediction",
journal="ASTRONOMY & ASTROPHYSICS",
year="2010",
volume="2010 (513)",
number="5",
month="February",
pages="49--56",
issn="0004-6361"
}