Predicting the corona for the 21 August 2017 total solar eclipse

Kód výsledku v IS VaVaI

<a href="https://www.isvavai.cz/riv?ss=detail&h=RIV%2F00216305%3A26210%2F18%3APU130479" target="_blank" >RIV/00216305:26210/18:PU130479 - isvavai.cz</a>

Výsledek na webu

<a href="https://apps.webofknowledge.com/full_record.do?product=WOS&search_mode=GeneralSearch&qid=1&SID=F45YR22i1Aw8DVwHPXd&page=1&doc=1" target="_blank" >https://apps.webofknowledge.com/full_record.do?product=WOS&search_mode=GeneralSearch&qid=1&SID=F45YR22i1Aw8DVwHPXd&page=1&doc=1</a>

DOI - Digital Object Identifier

<a href="http://dx.doi.org/10.1038/s41550-018-0562-5" target="_blank" >10.1038/s41550-018-0562-5</a>

Jazyk výsledku

angličtina

Název v původním jazyce

Predicting the corona for the 21 August 2017 total solar eclipse

Popis výsledku v původním jazyce

The total solar eclipse that occurred on 21 August 2017 across the United States provided an opportunity to test a magnetohydrodynamic model of the solar corona driven by measured magnetic fields. We used a new heating model based on the dissipation of Alfven waves, and a new energization mechanism to twist the magnetic field in filament channels. We predicted what the corona would look like one week before the eclipse. Here, we describe how this prediction was accomplished, and show that it compared favourably with observations of the eclipse in white light and extreme ultraviolet. The model allows us to understand the relationship of observed features, including streamers, corona! holes, prominences, polar plumes and thin rays, to the magnetic field. We show that the discrepancies between the model and observations arise from limitations in our ability to observe the Sun's magnetic field. Predictions of this kind provide opportunities to improve the models, forging the path to improved space weather prediction.

Název v anglickém jazyce

Predicting the corona for the 21 August 2017 total solar eclipse

Popis výsledku anglicky

The total solar eclipse that occurred on 21 August 2017 across the United States provided an opportunity to test a magnetohydrodynamic model of the solar corona driven by measured magnetic fields. We used a new heating model based on the dissipation of Alfven waves, and a new energization mechanism to twist the magnetic field in filament channels. We predicted what the corona would look like one week before the eclipse. Here, we describe how this prediction was accomplished, and show that it compared favourably with observations of the eclipse in white light and extreme ultraviolet. The model allows us to understand the relationship of observed features, including streamers, corona! holes, prominences, polar plumes and thin rays, to the magnetic field. We show that the discrepancies between the model and observations arise from limitations in our ability to observe the Sun's magnetic field. Predictions of this kind provide opportunities to improve the models, forging the path to improved space weather prediction.

Druh

J_imp - Článek v periodiku v databázi Web of Science

CEP obor

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OECD FORD obor

10308 - Astronomy (including astrophysics,space science)

Projekt

—

Návaznosti

S - Specificky vyzkum na vysokych skolach

Rok uplatnění

2018

Kód důvěrnosti údajů

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

Název periodika

NATURE ASTRONOMY

ISSN

2397-3366

e-ISSN

—

Svazek periodika

2

Číslo periodika v rámci svazku

11

Stát vydavatele periodika

GB - Spojené království Velké Británie a Severního Irska

Počet stran výsledku

9

Strana od-do

913-921

Kód UT WoS článku

000448876900022

EID výsledku v databázi Scopus

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