Astronomy and Astrophysics – Astrophysics
Scientific paper
May 2001
adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2001agusm..sp52b06s&link_type=abstract
American Geophysical Union, Spring Meeting 2001, abstract #SP52B-06
Astronomy and Astrophysics
Astrophysics
7500 Solar Physics, Astrophysics, And Astronomy, 7507 Chromosphere, 7509 Corona, 7546 Transition Region
Scientific paper
An alternative explanation of the coronal heating problem is the view that the solar corona is a result of a non-Maxwellian particle distribution generated in the chromosphere-transition zone, with a non-thermal tail modeled by a kappa function. The temperature increase is formed by the process of velocity filtration in the effective electric and gravitational potential experienced by the particles. This model, proposed by Scudder in 1992, makes specific predictions of the height-dependent density ne(h) distribution that become now testable with high-resolution soft X-ray and EUV data from Yohkoh, SoHO, and TRACE. In particular the density should vary as an inverse power law with altitude rather than decreasing exponentially as in the case of plasmas with Maxwellian velocity distributions. We employ two methods to determine the height dependence of the electron density in the solar corona: (1) from the background-subtracted EUV emission measure of loops observed above the solar limb with high resolution and narrow temperature filters (TRACE, EIT), and (2) from line-of-sight integrated differential emission measure [DEM(T)] modeling of quiet-Sun soft X-ray and EUV fluxes observed above the limb with narrow (TRACE, EIT) and broadband filters (Yohkoh). We fit the density models predicted by the velocity filtration model to determine the ranges of kappa-values that are consistent with the observations and attempt to discriminate the velocity filtration model from heating models.
Ascwanden M. J.
Scudder Jack D.
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