Multi-temperature Observations of Solar Microflares using RHESSI and SDO/AIA

Details Multi-temperature Observations of Solar Microflares using RHESSI and SDO/AIA Multi-temperature Observations of Solar Microflares using RHESSI and SDO/AIA

Dec 2010

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2010agufmsh23a1831m&link_type=abstract

American Geophysical Union, Fall Meeting 2010, abstract #SH23A-1831

Astronomy and Astrophysics

Astrophysics

[7519] Solar Physics, Astrophysics, And Astronomy / Flares, [7549] Solar Physics, Astrophysics, And Astronomy / Ultraviolet Emissions, [7554] Solar Physics, Astrophysics, And Astronomy / X-Rays, Gamma Rays, And Neutrinos, [7594] Solar Physics, Astrophysics, And Astronomy / Instruments And Techniques

Scientific paper

In this work, we estimate the Differential Emission Measure for solar microflares using data from the AIA instrument on SDO and RHESSI data. Seven of the AIA wavelength bands (94, 131, 171, 193, 304, and 335 Angstroms), which detect emission from solar plasma with temperatures ranging from less than 20,000 K to as high as 20 MK, are useful for this calculation. The RHESSI instrument observes solar flare plasma in the temperature range above 8 MK. Preliminary results for a microflare observed on 11 July 2010 show loop footpoint sources with broad emission measure distributions, with both low (<100,000 K) and high (>10 MK) plasma. There is also a loop visible in the AIA 131 and 94 Angstrom wavelength bands, which are sensitive to high temperatures. RHESSI images in the energy range between 4 and 10 keV also show the loop, which has a relatively narrow (in temperature) emission measure distribution, concentrated above 10 MK. Implications for flare heating scenarios which may result in this sort of emission measure distribution will be discussed.

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