A Two-Sided-Loop X-Ray Solar Coronal Jet Driven by a Minifilament Eruption. (arXiv:1811.05557v1 [astro-ph.SR])
<a href="http://arxiv.org/find/astro-ph/1/au:+Sterling_A/0/1/0/all/0/1">Alphonse C. Sterling</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Harra_L/0/1/0/all/0/1">Louise K. Harra</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Moore_R/0/1/0/all/0/1">Ronald L. Moore</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Falconer_D/0/1/0/all/0/1">David A. Falconer</a>
Most of the commonly discussed solar coronal jets are of the type consisting
of a single spire extending approximately vertically from near the solar
surface into the corona. Recent research supports that eruption of a miniature
filament (minifilament) drives many such single-spire jets, and concurrently
generates a miniflare at the eruption site. A different type of coronal jet,
identified in X-ray images during the Yohkoh era, are two-sided-loop jets,
which extend from a central excitation location in opposite directions, along
low-lying coronal loops more-or-less horizontal to the surface. We observe such
a two-sided-loop jet from the edge of active region (AR) 12473, using data from
Hinode XRT and EIS, and SDO AIA and HMI. Similar to single-spire jets, this
two-sided-loop jet results from eruption of a minifilament, which accelerates
to over 140 km/s before abruptly stopping after striking overlying
nearly-horizontal loop field at about 30,000 km altitude and producing the
two-sided-loop jet. Analysis of EIS raster scans show that a hot brightening,
consistent with a small flare, develops in the aftermath of the eruption, and
that Doppler motions (approx 40 km/s) occur near the jet-formation region. As
with many single-spire jets, the magnetic trigger here is apparently flux
cancelation, which occurs at a rate of approx 4×10^18 Mx/hr, comparable to the
rate observed in some single-spire AR jets. An apparent increase in the
(line-of-sight) flux occurs within minutes of onset of the minifilament
eruption, consistent with the apparent increase being due to a rapid
reconfiguration of low-lying field during and soon after minifilament-eruption
onset.
Most of the commonly discussed solar coronal jets are of the type consisting
of a single spire extending approximately vertically from near the solar
surface into the corona. Recent research supports that eruption of a miniature
filament (minifilament) drives many such single-spire jets, and concurrently
generates a miniflare at the eruption site. A different type of coronal jet,
identified in X-ray images during the Yohkoh era, are two-sided-loop jets,
which extend from a central excitation location in opposite directions, along
low-lying coronal loops more-or-less horizontal to the surface. We observe such
a two-sided-loop jet from the edge of active region (AR) 12473, using data from
Hinode XRT and EIS, and SDO AIA and HMI. Similar to single-spire jets, this
two-sided-loop jet results from eruption of a minifilament, which accelerates
to over 140 km/s before abruptly stopping after striking overlying
nearly-horizontal loop field at about 30,000 km altitude and producing the
two-sided-loop jet. Analysis of EIS raster scans show that a hot brightening,
consistent with a small flare, develops in the aftermath of the eruption, and
that Doppler motions (approx 40 km/s) occur near the jet-formation region. As
with many single-spire jets, the magnetic trigger here is apparently flux
cancelation, which occurs at a rate of approx 4×10^18 Mx/hr, comparable to the
rate observed in some single-spire AR jets. An apparent increase in the
(line-of-sight) flux occurs within minutes of onset of the minifilament
eruption, consistent with the apparent increase being due to a rapid
reconfiguration of low-lying field during and soon after minifilament-eruption
onset.
http://arxiv.org/icons/sfx.gif
