Blue-wing enhancement of the chromospheric Mg II h and k lines in a solar flare

Kód výsledku v IS VaVaI

<a href="https://www.isvavai.cz/riv?ss=detail&h=RIV%2F67985815%3A_____%2F18%3A00499723" target="_blank" >RIV/67985815:_____/18:00499723 - isvavai.cz</a>

Výsledek na webu

<a href="http://dx.doi.org/10.1093/pasj/psy047" target="_blank" >http://dx.doi.org/10.1093/pasj/psy047</a>

DOI - Digital Object Identifier

<a href="http://dx.doi.org/10.1093/pasj/psy047" target="_blank" >10.1093/pasj/psy047</a>

Jazyk výsledku

angličtina

Název v původním jazyce

Blue-wing enhancement of the chromospheric Mg II h and k lines in a solar flare

Popis výsledku v původním jazyce

We performed coordinated observations of AR 12205, which showed a C-class flare on 2014 November 11, with the Interface Region Imaging Spectrograph (IRIS) and the Domeless Solar Telescope (DST) at Hida Observatory. Cloud modeling of the Mg II h line suggests that the blue-wing enhancement with such a peak difference could have been caused by a chromospheric-temperature (cool) upflow. We discuss a scenario in which an upflow of cool plasma is lifted up by expanding hot plasma owing to the deep penetration of non-thermal electrons into the chromosphere. Furthermore, we found that the blueshift persisted without any subsequent redshift in the leading edge of the flare kernel during its decaying phase. The cause of such a long-lasting blueshift is also discussed.

Název v anglickém jazyce

Blue-wing enhancement of the chromospheric Mg II h and k lines in a solar flare

Popis výsledku anglicky

We performed coordinated observations of AR 12205, which showed a C-class flare on 2014 November 11, with the Interface Region Imaging Spectrograph (IRIS) and the Domeless Solar Telescope (DST) at Hida Observatory. Cloud modeling of the Mg II h line suggests that the blue-wing enhancement with such a peak difference could have been caused by a chromospheric-temperature (cool) upflow. We discuss a scenario in which an upflow of cool plasma is lifted up by expanding hot plasma owing to the deep penetration of non-thermal electrons into the chromosphere. Furthermore, we found that the blueshift persisted without any subsequent redshift in the leading edge of the flare kernel during its decaying phase. The cause of such a long-lasting blueshift is also discussed.

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

<a href="/cs/project/GA16-18495S" target="_blank" >GA16-18495S: Pokročilý výzkum Slunce se satelitem IRIS</a><br>

Návaznosti

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

Rok uplatnění

2018

Kód důvěrnosti údajů

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

Název periodika

Publications of the Astronomical Society of Japan

ISSN

0004-6264

e-ISSN

—

Svazek periodika

70

Číslo periodika v rámci svazku

6

Stát vydavatele periodika

JP - Japonsko

Počet stran výsledku

15

Strana od-do

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Kód UT WoS článku

000456072300002

EID výsledku v databázi Scopus

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