Multi-thermal atmosphere of a mini-solar flare during magnetic reconnection observed with IRIS
The result's identifiers
Result code in IS VaVaI
<a href="https://www.isvavai.cz/riv?ss=detail&h=RIV%2F67985815%3A_____%2F21%3A00548092" target="_blank" >RIV/67985815:_____/21:00548092 - isvavai.cz</a>
Result on the web
<a href="http://hdl.handle.net/11104/0324208" target="_blank" >http://hdl.handle.net/11104/0324208</a>
DOI - Digital Object Identifier
<a href="http://dx.doi.org/10.1051/0004-6361/202039229" target="_blank" >10.1051/0004-6361/202039229</a>
Alternative languages
Result language
angličtina
Original language name
Multi-thermal atmosphere of a mini-solar flare during magnetic reconnection observed with IRIS
Original language description
The aim of this work is to study the fine structure and dynamics of the plasma at a jet base forming a mini-flare between two emerging magnetic fluxes (EMFs) observed with IRIS and the Solar Dynamics Observatory instruments.Methods. We proceed to a spatio-temporal analysis of IRIS spectra observed in the spectral ranges of Mg II, C II, and Si IV ions. Doppler velocities from Mg II lines were computed using a cloud model technique.Results. Strong asymmetric Mg II and C II line profiles with extended blue wings observed at the reconnection site (jet base) are interpreted by the presence of two chromospheric temperature clouds: one explosive cloud with blueshifts at 290 km s(-1) and one cloud with smaller Doppler shift (around 36 km s(-1)). Simultaneously at the same location (jet base), strong emission of several transition region lines (e.g. O IV and Si IV), emission of the Mg II triplet lines, and absorption of identified chromospheric lines in Si IV broad profiles have been observed and analysed.Conclusions. Such observations of IRIS line and continuum emissions allow us to propose a stratification model for the white light, mini-flare atmosphere with multiple layers of different temperatures along the line of sight in a reconnection current sheet. It is the first time that we could quantify the fast speed (possibly Alfvenic flows) of cool clouds ejected perpendicularly to the jet direction via the cloud model technique. We conjecture that the ejected clouds come from plasma which was trapped between the two EMFs before reconnection or be caused by chromospheric-temperature (cool) upflow material similar to a surge during reconnection.
Czech name
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Czech description
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Classification
Type
J<sub>imp</sub> - Article in a specialist periodical, which is included in the Web of Science database
CEP classification
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OECD FORD branch
10308 - Astronomy (including astrophysics,space science)
Result continuities
Project
<a href="/en/project/GA19-09489S" target="_blank" >GA19-09489S: Advanced modelling of solar flare processes and their chromospheric emission</a><br>
Continuities
I - Institucionalni podpora na dlouhodoby koncepcni rozvoj vyzkumne organizace
Others
Publication year
2021
Confidentiality
S - Úplné a pravdivé údaje o projektu nepodléhají ochraně podle zvláštních právních předpisů
Data specific for result type
Name of the periodical
Astronomy & Astrophysics
ISSN
0004-6361
e-ISSN
1432-0746
Volume of the periodical
645
Issue of the periodical within the volume
January
Country of publishing house
FR - FRANCE
Number of pages
19
Pages from-to
A80
UT code for WoS article
000609886600001
EID of the result in the Scopus database
2-s2.0-85099714631