New types of the chromospheric anemone microflares: Case study. (arXiv:1904.09439v1 [astro-ph.SR])
<a href="http://arxiv.org/find/astro-ph/1/au:+Dumin_Y/0/1/0/all/0/1">Yu. V. Dumin</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Somov_B/0/1/0/all/0/1">B. V. Somov</a>
Context: The chromospheric anemone microflares (AMF) are an interesting kind
of the transient solar phenomena where the emission regions have a multi-ribbon
configuration, as distinct from the ordinary flares usually possessing only two
ribbons. The previously reported AMFs had typically three or, less frequently,
four ribbons; and it was shown in our recent Letter [Yu.V. Dumin & B.V. Somov,
A&A, 623, L4 (2019)] that they can be reasonably described by the so-called
GKSS model of magnetic field, involving four magnetic sources with various
polarity and arrangement. Aims: An interesting question is if one can see more
complex types of AMF (containing the grater number of the emission ribbons),
which might be produced by more elaborated magnetic configurations? Methods: To
answer this question, we performed a visual inspection of the large set of the
emission patterns in the chromospheric line CaII H recorded by Hinode/SOT and
confronted them with the respective magnetograms obtained by SDO/HMI. Results:
As follows from our analysis, it is really possible to identify the AMFs with
much more complex spatial configurations as compared to the previously-known
ones, e.g., involving five luminous ribbons with a nontrivial arrangement. They
are produced by the effective magnetic sources (sunspots) of different polarity
with intermittent arrangement in the cross-like configuration, but their number
is greater than in the standard GKSS model.
Context: The chromospheric anemone microflares (AMF) are an interesting kind
of the transient solar phenomena where the emission regions have a multi-ribbon
configuration, as distinct from the ordinary flares usually possessing only two
ribbons. The previously reported AMFs had typically three or, less frequently,
four ribbons; and it was shown in our recent Letter [Yu.V. Dumin & B.V. Somov,
A&A, 623, L4 (2019)] that they can be reasonably described by the so-called
GKSS model of magnetic field, involving four magnetic sources with various
polarity and arrangement. Aims: An interesting question is if one can see more
complex types of AMF (containing the grater number of the emission ribbons),
which might be produced by more elaborated magnetic configurations? Methods: To
answer this question, we performed a visual inspection of the large set of the
emission patterns in the chromospheric line CaII H recorded by Hinode/SOT and
confronted them with the respective magnetograms obtained by SDO/HMI. Results:
As follows from our analysis, it is really possible to identify the AMFs with
much more complex spatial configurations as compared to the previously-known
ones, e.g., involving five luminous ribbons with a nontrivial arrangement. They
are produced by the effective magnetic sources (sunspots) of different polarity
with intermittent arrangement in the cross-like configuration, but their number
is greater than in the standard GKSS model.
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