Astronomy and Astrophysics – Astronomy
Scientific paper
Jul 2006
adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2006apj...646l..81a&link_type=abstract
The Astrophysical Journal, Volume 646, Issue 1, pp. L81-L84.
Astronomy and Astrophysics
Astronomy
7
Sun: Corona, Sun: Magnetic Fields, Sun: Photosphere, Sun: X-Rays, Gamma Rays
Scientific paper
In this study, the soft X-ray luminosity of the solar corona, measured by the Yohkoh spacecraft for 104 well-developed and decaying active regions, is compared to the magnetic field parameters determined from SOHO MDI high-resolution magnetograms. We calculate and compare (1) two area-independent characteristics of the magnetic field: the index (α) of the magnetic power spectrum, E(k)~k-α, and the magnetic energy dissipation rate (ɛ¯/η), which is a proxy for the energy of random footpoint motions induced by turbulent convection in the photosphere and below; and (2) four area-independent parameters of the soft X-ray emission: the area-normalized flux in Yohkoh Al.1 and AlMgMn channels, and the emission measure and temperature of the coronal plasma. Here we report that the area-normalized soft X-ray flux correlates with both the power index α (Pearson correlation coefficient ρ=0.72/Al.1 and 0.73/AlMgMn) and the magnetic energy dissipation rate ɛ¯/η (ρ=0.68/Al.1 and 0.70/AlMgMn). Also, both magnetic parameters are well-correlated with the logarithm of the emission measure (ρ=0.72) and the logarithm of temperature [ρ=0.59/α and 0.63/(ɛ¯/η)]. Our results present strong observational support to those coronal heating models that rely on random footpoint motions as an energy source to heat the corona above active regions.
Abramenko Valentina I.
Pevtsov Alexander
Romano Pado
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