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

Kód výsledku v 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>

Výsledek na webu

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DOI - Digital Object Identifier

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Jazyk výsledku

čeština

Název v původním jazyce

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

Popis výsledku v původním jazyce

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-

Název v anglickém jazyce

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

Popis výsledku anglicky

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-

Druh

J_x - Nezařazeno - Článek v odborném periodiku (Jimp, Jsc a Jost)

CEP obor

BN - Astronomie a nebeská mechanika, astrofyzika

OECD FORD obor

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Projekt

<a href="/cs/project/GA205%2F09%2F1469" target="_blank" >GA205/09/1469: Studium slunečních koronálních struktur a jejich dynamiky</a><br>

Návaznosti

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

Rok uplatnění

2010

Kód důvěrnosti údajů

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

Název periodika

ASTRONOMY & ASTROPHYSICS

ISSN

0004-6361

e-ISSN

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Svazek periodika

2010 (513)

Číslo periodika v rámci svazku

5

Stát vydavatele periodika

FR - Francouzská republika

Počet stran výsledku

7

Strana od-do

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Kód UT WoS článku

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EID výsledku v databázi Scopus

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