Spatially resolved signatures of bi-directional flows observed in inverted-Y shaped jets. (arXiv:1908.05132v1 [astro-ph.SR])
<a href="http://arxiv.org/find/astro-ph/1/au:+Nelson_C/0/1/0/all/0/1">C. J. Nelson</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Freij_N/0/1/0/all/0/1">N. Freij</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Bennett_S/0/1/0/all/0/1">S. Bennett</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Erdelyi_R/0/1/0/all/0/1">R. Erdélyi</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Mathioudakis_M/0/1/0/all/0/1">M. Mathioudakis</a>
Numerous apparent signatures of magnetic reconnection have been reported in
the solar photosphere, including inverted-Y shaped jets. The reconnection at
these sites is expected to cause localised bi-directional flows and extended
shock waves; however, these signatures are rarely observed as extremely high
spatial-resolution data are required. Here, we use H-alpha imaging data sampled
by the Swedish Solar Telescope’s CRisp Imaging SpectroPolarimeter to
investigate whether bi-directional flows can be detected within inverted-Y
shaped jets near the solar limb. These jets are apparent in the H-alpha line
wings, while no signature of either jet is observed in the H-alpha line core,
implying reconnection took place below the chromospheric canopy. Asymmetries in
the H-alpha line profiles along the legs of the jets indicate the presence of
bi-directional flows, consistent with cartoon models of reconnection in
chromospheric anemone jets. These asymmetries are present for over two minutes,
longer than the lifetimes of Rapid Blue Excursions, and beyond pm 1 AA into
the wings of the line indicating that flows within the inverted-Y shaped jets
are responsible for the imbalance in the profiles, rather than motions in the
foreground. Additionally, surges form following the occurrence of the
inverted-Y shaped jets. This surge formation is consistent with models which
suggest such events could be caused by the propagation of shock waves from
reconnection sites in the photosphere to the upper atmosphere. Overall, our
results provide evidence that magnetic reconnection in the photosphere can
cause bi-directional flows within inverted-Y shaped jets and could be the
driver of surges.
Numerous apparent signatures of magnetic reconnection have been reported in
the solar photosphere, including inverted-Y shaped jets. The reconnection at
these sites is expected to cause localised bi-directional flows and extended
shock waves; however, these signatures are rarely observed as extremely high
spatial-resolution data are required. Here, we use H-alpha imaging data sampled
by the Swedish Solar Telescope’s CRisp Imaging SpectroPolarimeter to
investigate whether bi-directional flows can be detected within inverted-Y
shaped jets near the solar limb. These jets are apparent in the H-alpha line
wings, while no signature of either jet is observed in the H-alpha line core,
implying reconnection took place below the chromospheric canopy. Asymmetries in
the H-alpha line profiles along the legs of the jets indicate the presence of
bi-directional flows, consistent with cartoon models of reconnection in
chromospheric anemone jets. These asymmetries are present for over two minutes,
longer than the lifetimes of Rapid Blue Excursions, and beyond pm 1 AA into
the wings of the line indicating that flows within the inverted-Y shaped jets
are responsible for the imbalance in the profiles, rather than motions in the
foreground. Additionally, surges form following the occurrence of the
inverted-Y shaped jets. This surge formation is consistent with models which
suggest such events could be caused by the propagation of shock waves from
reconnection sites in the photosphere to the upper atmosphere. Overall, our
results provide evidence that magnetic reconnection in the photosphere can
cause bi-directional flows within inverted-Y shaped jets and could be the
driver of surges.
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