Comparing eclipse observations of the 2008 August 1 solar corona with an MHD model prediction

Result code in IS VaVaI

<a href="https://www.isvavai.cz/riv?ss=detail&h=RIV%2F00216305%3A26210%2F10%3APU88267" target="_blank" >RIV/00216305:26210/10:PU88267 - isvavai.cz</a>

Result on the web

—

DOI - Digital Object Identifier

—

Result language

čeština

Original language name

Comparing eclipse observations of the 2008 August 1 solar corona with an MHD model prediction

Original language 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-

Czech name

Comparing eclipse observations of the 2008 August 1 solar corona with an MHD model prediction

Czech 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-

Type

J_x - Unclassified - Peer-reviewed scientific article (Jimp, Jsc and Jost)

CEP classification

BN - Astronomy and celestial mechanics, astrophysics

OECD FORD branch

—

Project

<a href="/en/project/GA205%2F09%2F1469" target="_blank" >GA205/09/1469: Study of solar coronal structures and their dynamics</a><br>

Continuities

P - Projekt vyzkumu a vyvoje financovany z verejnych zdroju (s odkazem do CEP)

Publication year

2010

Confidentiality

S - Úplné a pravdivé údaje o projektu nepodléhají ochraně podle zvláštních právních předpisů

Name of the periodical

ASTRONOMY & ASTROPHYSICS

ISSN

0004-6361

e-ISSN

—

Volume of the periodical

2010 (513)

Issue of the periodical within the volume

5

Country of publishing house

FR - FRANCE

Number of pages

7

Pages from-to

—

UT code for WoS article

—

EID of the result in the Scopus database

—