RHESSI Investigations of the Neupert Effect in Solar Flares

Details RHESSI Investigations of the Neupert Effect in Solar Flares RHESSI Investigations of the Neupert Effect in Solar Flares

Dec 2002

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2002aas...20114101b&link_type=abstract

American Astronomical Society Meeting 201, #141.01; Bulletin of the American Astronomical Society, Vol. 35, p.566

Astronomy and Astrophysics

Astronomy

2

Scientific paper

In many solar flares, the time integral of the hard X-ray emission closely matches the temporal variation of the soft X-ray emission. This is known as the Neupert Effect and is believed to result when the same accelerated electrons that produce the bremsstrahlung hard X-rays also heat the plasma that produces the thermal-bremsstrahlung soft X-rays. The Reuven Ramaty High Energy Solar Spectroscopic Imager (RHESSI) is uniquely capable of investigating this effect since it covers soft X-rays (down to 3 keV) and hard X-rays with keV energy resolution, arcsecond-class angular resolution, and sub-second time resolution. Quantifying the significance of this relationship requires the use of statistical techniques to relate the hard X-ray flux to the derivative of the soft X-ray time line. The difficulty is in accounting for the statistical noise in the data and in deciding what smoothing time scale to use in computing the derivative. These problems can be resolved by using the wavelet correlation of the two light curves. The wavelet we use is the derivative of a smoothing function. The smoothing time scale and the statistical noise in the data are naturally accounted for by the wavelet transform. Then we can give a significance level for the agreement of the data with the Neupert Effect.

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