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

Result code in 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>
Result on the web
<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>

Result language
angličtina
Original language name
Blue-wing enhancement of the chromospheric Mg II h and k lines in a solar flare
Original language description
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.
Czech name
—
Czech description
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Type
J<sub>imp</sub> - Article in a specialist periodical, which is included in the Web of Science database
CEP classification
—
OECD FORD branch
10308 - Astronomy (including astrophysics,space science)

Project
<a href="/en/project/GA16-18495S" target="_blank" >GA16-18495S: Advanced solar science with IRIS</a><br>
Continuities
P - Projekt vyzkumu a vyvoje financovany z verejnych zdroju (s odkazem do CEP)

Publication year
2018
Confidentiality
S - Úplné a pravdivé údaje o projektu nepodléhají ochraně podle zvláštních právních předpisů

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