Statistics – Computation
Scientific paper
May 2011
adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2011aas...21832202s&link_type=abstract
American Astronomical Society, AAS Meeting #218, #322.02; Bulletin of the American Astronomical Society, Vol. 43, 2011
Statistics
Computation
Scientific paper
It is well known that solar flare energies have a self-similar distribution. The number of flares, N, of any given energy, E, follows a power-law distribution, dN/dE E^(-alpha), over many orders of magnitude, with alpha 1.8. A similar distribution holds for stellar coronae, but in this case, typically alpha > 2. The value alpha=2 is important because it represents a threshold beyond which it is possible to ascribe all of the coronal luminosity to increasingly weaker, but more numerous, flares.
Current methods to evaluate the flare distribution index alpha for stars are limited by two factors: they either depend on explicit detections of flares, or if the flare distribution itself is being modeled, then they are highly computation intensive and are thus slow. We have developed analytical methodology that substitutes for Monte Carlo simulations over a majority of the latter calculations. This causes improvements in computational speed of over 100x. We describe these methods below, and apply it to some simulated and observed data.
This work was supported by CXC NASA contract NAS8-39073 and Chandra grant AR0-11001X.
Connors Alanna
Drake Jeremy J.
Kashyap Vinay
Reeves Katharine K.
Saar Steven H.
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