A White-light Flare Powered by Magnetic Reconnection in the Lower Solar Atmosphere. (arXiv:2003.11747v1 [astro-ph.SR])
<a href="http://arxiv.org/find/astro-ph/1/au:+Song_Y/0/1/0/all/0/1">Yongliang Song</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Tian_H/0/1/0/all/0/1">Hui Tian</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Zhu_X/0/1/0/all/0/1">Xiaoshuai Zhu</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Chen_Y/0/1/0/all/0/1">Yajie Chen</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Zhang_M/0/1/0/all/0/1">Mei Zhang</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Zhang_J/0/1/0/all/0/1">Jingwen Zhang</a>

White-light flares (WLFs), first observed in 1859, refer to a type of solar
flares showing an obvious enhancement of the visible continuum emission. This
type of enhancement often occurs in most energetic flares, and is usually
interpreted as a consequence of efficient heating in the lower solar atmosphere
through non-thermal electrons propagating downward from the energy release site
in the corona. However, this coronal-reconnection model has difficulty in
explaining the recently discovered small WLFs. Here we report a C2.3
white-light flare, which are associated with several observational phenomena:
fast decrease in opposite-polarity photospheric magnetic fluxes, disappearance
of two adjacent pores, significant heating of the lower chromosphere,
negligible increase of hard X-ray flux, and an associated U-shaped magnetic
field configuration. All these suggest that this white-light flare is powered
by magnetic reconnection in the lower part of the solar atmosphere rather than
by reconnection higher up in the corona.

White-light flares (WLFs), first observed in 1859, refer to a type of solar
flares showing an obvious enhancement of the visible continuum emission. This
type of enhancement often occurs in most energetic flares, and is usually
interpreted as a consequence of efficient heating in the lower solar atmosphere
through non-thermal electrons propagating downward from the energy release site
in the corona. However, this coronal-reconnection model has difficulty in
explaining the recently discovered small WLFs. Here we report a C2.3
white-light flare, which are associated with several observational phenomena:
fast decrease in opposite-polarity photospheric magnetic fluxes, disappearance
of two adjacent pores, significant heating of the lower chromosphere,
negligible increase of hard X-ray flux, and an associated U-shaped magnetic
field configuration. All these suggest that this white-light flare is powered
by magnetic reconnection in the lower part of the solar atmosphere rather than
by reconnection higher up in the corona.

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