A Nanoflare Heating Model and Comparison with Observations

Details A Nanoflare Heating Model and Comparison with Observations A Nanoflare Heating Model and Comparison with Observations

Oct 2009

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2009apj...703.2118s&link_type=abstract

The Astrophysical Journal, Volume 703, Issue 2, pp. 2118-2130 (2009).

Astronomy and Astrophysics

Astronomy

5

Sun: Activity, Sun: Corona, Sun: Flares, Sun: X-Rays, Gamma Rays

Scientific paper

A nanoflare-heated coronal loop model is developed based on the model of Vekstein & Katsukawa. We performed numerical simulations based on the model, and then compared the results with the Yohkoh/Soft X-ray Telescope (SXT) and Transition Region and Coronal Explorer (TRACE) observations. We found that the most significant difference between hot (>2 MK) SXT loops and cool (~1 MK) TRACE loops is the energy of nanoflares and the magnetic field strength. Energy of individual nanoflares is 1024-25 erg for SXT loops, and 1023 erg for TRACE loops. This is derived from the observed intensity fluctuations. To observed mean intensities, we require the model SXT loops to have a stronger magnetic field than the TRACE loops, 40 G and 8 G, respectively. The model predicts two characteristic properties of nanoflare-heated coronal loops: (1) the SXT and TRACE light curves of a coronal loop show weak cross-correlation with a lag time corresponding to the cooling timescale. (2) SXT loops have a smaller volumetric filling factor than TRACE loops. We consider that this difference in the filling factor makes SXT loops look more diffuse than TRACE loops.

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