THERMODYNAMICS OF THE SOLAR CORONA AND EVOLUTION OF THE SOLAR MAGNETIC FIELD AS INFERRED FROM THE TOTAL SOLAR ECLIPSE OBSERVATIONS OF 2010 JULY 11

Kód výsledku v IS VaVaI

<a href="https://www.isvavai.cz/riv?ss=detail&h=RIV%2F00216305%3A26210%2F11%3APU93427" target="_blank" >RIV/00216305:26210/11:PU93427 - isvavai.cz</a>

Výsledek na webu

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DOI - Digital Object Identifier

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Jazyk výsledku

angličtina

Název v původním jazyce

THERMODYNAMICS OF THE SOLAR CORONA AND EVOLUTION OF THE SOLAR MAGNETIC FIELD AS INFERRED FROM THE TOTAL SOLAR ECLIPSE OBSERVATIONS OF 2010 JULY 11

Popis výsledku v původním jazyce

We report on the first multi-wavelength coronal observations, taken simultaneously in white light, H alpha 656.3 nm, Fe ix 435.9 nm, Fe x 637.4 nm, Fe xi 789.2 nm, Fe xiii 1074.7 nm, Fe xiv 530.3 nm, and Ni xv 670.2 nm, during the total solar eclipse of2010 July 11 from the atoll of Tatakoto in French Polynesia. The data enabled temperature differentiations as low as 0.2 x 106 K. The first-ever images of the corona in Fe ix and Ni xv showed that there was very little plasma below 5 x 105 K and above 2.5 x 106 K. The suite of multi-wavelength observations also showed that open field lines have an electron temperature near 1x106 K, while the hottest, 2x106 K, plasma resides in intricate loops forming the bulges of streamers, also known as cavities, as discovered in our previous eclipse observations. The eclipse images also revealed unusual coronal structures, in the form of ripples and streaks, produced by the passage of coronal mass ejections and eruptive prominences prior to totality,

Název v anglickém jazyce

THERMODYNAMICS OF THE SOLAR CORONA AND EVOLUTION OF THE SOLAR MAGNETIC FIELD AS INFERRED FROM THE TOTAL SOLAR ECLIPSE OBSERVATIONS OF 2010 JULY 11

Popis výsledku anglicky

We report on the first multi-wavelength coronal observations, taken simultaneously in white light, H alpha 656.3 nm, Fe ix 435.9 nm, Fe x 637.4 nm, Fe xi 789.2 nm, Fe xiii 1074.7 nm, Fe xiv 530.3 nm, and Ni xv 670.2 nm, during the total solar eclipse of2010 July 11 from the atoll of Tatakoto in French Polynesia. The data enabled temperature differentiations as low as 0.2 x 106 K. The first-ever images of the corona in Fe ix and Ni xv showed that there was very little plasma below 5 x 105 K and above 2.5 x 106 K. The suite of multi-wavelength observations also showed that open field lines have an electron temperature near 1x106 K, while the hottest, 2x106 K, plasma resides in intricate loops forming the bulges of streamers, also known as cavities, as discovered in our previous eclipse observations. The eclipse images also revealed unusual coronal structures, in the form of ripples and streaks, produced by the passage of coronal mass ejections and eruptive prominences prior to totality,

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

2011

Kód důvěrnosti údajů

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

Název periodika

ASTROPHYSICAL JOURNAL

ISSN

0004-637X

e-ISSN

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Svazek periodika

734

Číslo periodika v rámci svazku

1

Stát vydavatele periodika

US - Spojené státy americké

Počet stran výsledku

18

Strana od-do

120-137

Kód UT WoS článku

000291386500048

EID výsledku v databázi Scopus

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