Topological model of the anemone microflares in the solar chromosphere. (arXiv:1811.06214v1 [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>
The chromospheric anemone microflares, which were discovered by Hinode
satellite about a decade ago, are the specific transient phenomena starting
from a few luminous ribbons on the chromospheric surface and followed by the
eruption upwards. While the eruptive stage was studied in sufficient detail, a
quantitative theory of formation of the initial multi-ribbon structure remains
undeveloped till now. Here, we construct a sufficiently simple but general
model of the magnetic field sources that is able to reproduce all the observed
types of the luminous ribbons by varying only a single parameter. As a working
tool, we employ the Gorbachev-Kel’ner-Somov-Shvarts (GKSS) model of the
magnetic field, which was originally suggested about three decades ago to
explain fast ignition of the magnetic reconnection over considerable spatial
scales by tiny displacements of the magnetic sources. Quite unexpectedly, this
model turns out to be efficient also for the description of generic
multi-ribbon structure in the anemone flares. As follows from our numerical
simulation, displacement of a single magnetic source (sunspot) with respect to
three other sources results in a complex transformation from three to four
ribbons and, then, again to three ribbons but with an absolutely different
arrangement. Such structures closely remind the observed patterns of emission
in the anemone microflares.
The chromospheric anemone microflares, which were discovered by Hinode
satellite about a decade ago, are the specific transient phenomena starting
from a few luminous ribbons on the chromospheric surface and followed by the
eruption upwards. While the eruptive stage was studied in sufficient detail, a
quantitative theory of formation of the initial multi-ribbon structure remains
undeveloped till now. Here, we construct a sufficiently simple but general
model of the magnetic field sources that is able to reproduce all the observed
types of the luminous ribbons by varying only a single parameter. As a working
tool, we employ the Gorbachev-Kel’ner-Somov-Shvarts (GKSS) model of the
magnetic field, which was originally suggested about three decades ago to
explain fast ignition of the magnetic reconnection over considerable spatial
scales by tiny displacements of the magnetic sources. Quite unexpectedly, this
model turns out to be efficient also for the description of generic
multi-ribbon structure in the anemone flares. As follows from our numerical
simulation, displacement of a single magnetic source (sunspot) with respect to
three other sources results in a complex transformation from three to four
ribbons and, then, again to three ribbons but with an absolutely different
arrangement. Such structures closely remind the observed patterns of emission
in the anemone microflares.
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