Spectral Characteristics and Formation Height of Off-limb Flare Ribbons
The result's identifiers
Result code in IS VaVaI
<a href="https://www.isvavai.cz/riv?ss=detail&h=RIV%2F67985815%3A_____%2F20%3A00534353" target="_blank" >RIV/67985815:_____/20:00534353 - isvavai.cz</a>
Result on the web
<a href="http://hdl.handle.net/11104/0313047" target="_blank" >http://hdl.handle.net/11104/0313047</a>
DOI - Digital Object Identifier
<a href="http://dx.doi.org/10.3847/1538-4357/ab9603" target="_blank" >10.3847/1538-4357/ab9603</a>
Alternative languages
Result language
angličtina
Original language name
Spectral Characteristics and Formation Height of Off-limb Flare Ribbons
Original language description
Flare ribbons are bright manifestations of flare energy dissipation in the lower solar atmosphere. For the first time, we report on high-resolution imaging spectroscopy observations of flare ribbons situated off limb in the H beta and Caii 8542 A lines and make a detailed comparison with radiative hydrodynamic simulations. Observations of the X8.2 class solar flare SOL 2017-09-10T16:06 UT obtained with the Swedish Solar Telescope reveal bright horizontal emission layers in H beta line-wing images located near the footpoints of the flare loops. The apparent separation between the ribbon observed in the H beta wing and the nominal photospheric limb is about 300-500 km. The Caii 8542 A line-wing images show much fainter ribbon emissions located right on the edge of the limb, without clear separation from the limb. RADYN models are used to investigate synthetic spectral line profiles for the flaring atmosphere, and good agreement is found with the observations. The simulations show that, toward the limb, where the line of sight is substantially oblique with respect to the vertical direction, the flaring atmosphere model reproduces the high contrast of the off-limb H beta ribbons and their significant elevation above the photosphere. The ribbons in the Caii 8542 A line-wing images are located deeper in the lower solar atmosphere with a lower contrast. A comparison of the height deposition of electron beam energy and the intensity contribution function shows that the H beta line-wing intensities can be a useful tracer of flare energy deposition in the lower solar atmosphere.
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
2020
Confidentiality
S - Úplné a pravdivé údaje o projektu nepodléhají ochraně podle zvláštních právních předpisů
Data specific for result type
Name of the periodical
Astrophysical Journal
ISSN
1538-4357
e-ISSN
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Volume of the periodical
896
Issue of the periodical within the volume
2
Country of publishing house
US - UNITED STATES
Number of pages
14
Pages from-to
120
UT code for WoS article
000543365200001
EID of the result in the Scopus database
2-s2.0-85086857904