A Test of a New Flare Loop Scaling Law Using YOHKOH SXT and GOES Observations

Details A Test of a New Flare Loop Scaling Law Using YOHKOH SXT and GOES Observations A Test of a New Flare Loop Scaling Law Using YOHKOH SXT and GOES Observations

May 1996

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1996apj...462..977m&link_type=abstract

Astrophysical Journal v.462, p.977

Astronomy and Astrophysics

Astronomy

10

Stars: Activity, Stars: Flare, Stars: Magnetic Fields, Sun: Flares, Sun: X-Rays, Gamma Rays, X-Rays: Stars

Scientific paper

We compare the lengths of coronal loops observed on the Sun using the Soft X-Ray Telescope on Yohkoh with those predicted from the theoretical model of Hawley et al. This model relates the temporal behavior of coronal emission observed during flares on active stars to the length of the loops undergoing flaring. In that model, the footpoint-to-footpoint loop length 2L (measured in kilometers) should obey the relationship 2L ≃ 0.01Y where Y = l.25πr3/7τd4/7TA½, τr is the "rise time" (in seconds) from flare onset to flare peak, τd is the "decay time" (s) from flare peak to the time when the emission measure is 25% of its peak value, and TA (K) is the temperature at the top of the loop at flare peak. The observations show a strong correlation between 2L and Y, with the theoretical relationship consistent with observed loop lengths in most cases. For a few loops, the theoretical model tends to somewhat over-predict the loop length. When the observed loop lengths are fitted to a single power-law relationship in Y, we find the data are best fitted by log 2L = log (0.44±0.06) + (0.75±0.05) log Y. We offer no quantitative theoretical justification for this relationship, but we do suggest several reasons why the Hawley et al. model over-predicts loop lengths in some cases.

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