Coronal Magnetic Field Topology from Total Solar Eclipse Observations
The result's identifiers
Result code in IS VaVaI
<a href="https://www.isvavai.cz/riv?ss=detail&h=RIV%2F00216305%3A26210%2F20%3APU136698" target="_blank" >RIV/00216305:26210/20:PU136698 - isvavai.cz</a>
Result on the web
<a href="https://iopscience.iop.org/article/10.3847/1538-4357/ab8ae6/pdf" target="_blank" >https://iopscience.iop.org/article/10.3847/1538-4357/ab8ae6/pdf</a>
DOI - Digital Object Identifier
<a href="http://dx.doi.org/10.3847/1538-4357/ab8ae6" target="_blank" >10.3847/1538-4357/ab8ae6</a>
Alternative languages
Result language
angličtina
Original language name
Coronal Magnetic Field Topology from Total Solar Eclipse Observations
Original language description
Measuring the global magnetic field of the solar corona remains exceptionally challenging. The fine-scale density structures observed in white-light images taken during total solar eclipses are currently the best proxies for inferring the magnetic field direction in the corona from the solar limb out to several solar radii (R). We present, for the first time, the topology of the coronal magnetic field continuously between 1 and 6 R, as quantitatively inferred with the rolling Hough transform for 14 unique eclipse coronae that span almost two complete solar cycles. We find that the direction of the coronal magnetic field does not become radial until at least 3 R, with a high variance between 1.5 and 3 R at different latitudes and phases of the solar cycle. We find that the most nonradial coronal field topologies occur above regions with weaker magnetic field strengths in the photosphere, while stronger photospheric fields are associated with highly radial field lines in the corona. In addition, we find an abundance of field lines that extend continuously from the solar surface out to several solar radii at all latitudes, regardless of the presence of coronal holes. These results have implications for testing and constraining coronal magnetic field models, and for linking in situ solar wind measurements to their sources at the Sun.
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
—
Continuities
S - Specificky vyzkum na vysokych skolach
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
0004-637X
e-ISSN
1538-4357
Volume of the periodical
895
Issue of the periodical within the volume
2
Country of publishing house
US - UNITED STATES
Number of pages
14
Pages from-to
123-137
UT code for WoS article
000539719500001
EID of the result in the Scopus database
2-s2.0-85086278743