AIA and RHESSI Observations of Solar Coronal Jets

Details AIA and RHESSI Observations of Solar Coronal Jets AIA and RHESSI Observations of Solar Coronal Jets

Dec 2010

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2010agufmsh23a1826k&link_type=abstract

American Geophysical Union, Fall Meeting 2010, abstract #SH23A-1826

Astronomy and Astrophysics

Astrophysics

[7519] Solar Physics, Astrophysics, And Astronomy / Flares, [7526] Solar Physics, Astrophysics, And Astronomy / Magnetic Reconnection, [7554] Solar Physics, Astrophysics, And Astronomy / X-Rays, Gamma Rays, And Neutrinos

Scientific paper

The broad temperature coverage and high time resolution of AIA observations provides an excellent diagnostic tool to study solar flares. We combine AIA EUV observations with RHESSI hard X-ray observations to study the geometry, time evolution, and energetics of solar coronal jets. We report on a jet event of 2010 July 20 2UT (GOES A5) that shows the standard jet geometry of interchange reconnection (e.g. Moore et al. 2010). The hard X-ray observations reveal a very compact (4"x4") thermal flare loop. Counts in the non-thermal range, however, are too low to make an image of the HXR footpoints. The jet itself is only seen at EUV wavelengths with a width of 15" and a length of 60". The EUV time evolution shows two components, one that closely follows the HXR time profile and a second one that lasts longer that represents the jet evolution. RHESSI temperature diagnostics of hot flare plasma nicely complements the three AIA filters (193A, 131A, and 94A) with temperature responses to hot plasma (>6 MK). The fit to the HXR spectrum reveals a peak temperature of 9.1 MK. For this temperature range, the filter ratio of 131A and 94A is unique and steeply increasing with temperature. The 131/94 ratio gives a peak temperatures around 9.9 MK with the same temperature trend as seen with RHESSI. This indicates that the presently available filter response curves for 131A and 94A can be used as temperature diagnostics of hot (6-18 MK) flare plasmas.

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