Modeling the Secondary Flare Irradiance Measured by Solar Dynamic Observatory (SDO) Extreme ultraviolet Variability Experiment (EVE)

Details Modeling the Secondary Flare Irradiance Measured by Solar Dynamic Observatory (SDO) Extreme ultraviolet Variability Experiment (EVE) Modeling the Secondary Flare Irradiance Measured by Solar Dynamic Observatory (SDO) Extreme ultraviolet Variability Experiment (EVE)

Dec 2010

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2010agufmsh13a..05h&link_type=abstract

American Geophysical Union, Fall Meeting 2010, abstract #SH13A-05

Astronomy and Astrophysics

Astrophysics

[7519] Solar Physics, Astrophysics, And Astronomy / Flares, [7538] Solar Physics, Astrophysics, And Astronomy / Solar Irradiance, [7549] Solar Physics, Astrophysics, And Astronomy / Ultraviolet Emissions

Scientific paper

NASA’s Solar Dynamic Observatory (SDO) launched on 11 February 2010 and normal operations for all three instruments began 1 May 2010. Since then numerous small and moderate (C- and M-class) flares have been observed. One interesting feature observed by the Extreme ultraviolet Variability Experiment (EVE) is the enhancement of 2-3 million K emission several hours after the flare’s soft x-ray emission. From the Atmospheric Imaging Assembly (AIA) images, we can tell that these secondary emissions occur in the same active region as the flare but not in same coronal loops. Here, we examine the C8.8 flare that occurred on 5 May 2010. The flare occurred in Active Region 11069, a small magnetically complex region near the western limb of the Sun. The gradual phase of the flare is clearly seen in both GOES soft X-rays and the hot coronal emissions (>2 million K) measured by EVE. The secondary flare emission starts 30 minutes after the peak in gradual phase and slowly increases over an hour before decaying to the pre-flare levels. It is most strongly seen in Fe XV and Fe XVI (2-3 million K). Using the Enthalpy-Based Thermal Evolution of Loops (EBTEL) model, we are able calculate the EUV irradiance of a set of coronal loops for a given heating function. This allows us to determine the best-fit heating profile as a function of time for the C8.8 flare. The heating profile for this event clearly shows that there are two separate phases of heating. The first phase involves traditional post-flare loops. The field reconnects after erupting, and the energy released during the reconnection heats the plasma to very high temperatures. As the loops cool, emissions are seen in progressively cooler lines from 10 to 1 million K. The second phase is very different. A large number of coronal loops are heated only modestly-. The plasma in each loop, instead of reaching 10 million K, reaches 3 million K. The heating is also spread out over an hour generating the long secondary flare emission profile. We discuss the nature of this secondary flare emission, which seems to be an important component of many events.

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