Astronomy and Astrophysics – Astrophysics
Scientific paper
May 1994
adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1994apj...427..446s&link_type=abstract
Astrophysical Journal, Part 1 (ISSN 0004-637X), vol. 427, no. 1, p. 446-452
Astronomy and Astrophysics
Astrophysics
53
Solar Atmosphere, Solar Corona, Solar Transition Region, Solar Wind, Electron Emission, Geopotential Height, Ion Emission, Magnetic Fields, Velocity Distribution
Scientific paper
The empirically observed number flux in the solar wind at 1 AU is used as a constraint on the number flux that must be available at the base of the transition region (TR) (kT approx. equal to 1.2 eV) to supply the steady solar wind. Using truncated kappa distributions, fK, as nonthermal prototypes, estimates have been obtained of the regimes of K+/- that provide sufficient and equal solar wind bound number fluxes for TR ions and electrons. The approximate regimes of the required ion and electron K values are given by inequalities: 2.06 less than K+ less than 2.69; and 2.62 less than K- less than 3.15. These intervals are wholly within and independent of previously published inferences (Scudder 1992a) of the nonthermal tail strengths at the base of the TR of the solar atmosphere from the excess ion Doppler widths and energy maintenance of the corona, respectively. Unlike the convected isotropic Gaussian distributions, these nonthermal fK with the indicated ranges of K can provide both the required, equal number and energy fluxes to be consistent with conserved quantities observed at 1 AU. A truncated Gaussian distribution can supply neither required flux value. With these findings it is concluded that the velocity filtration model of Scudder (1992a) is a viable, alternative model for the formation of the corona that is considerably more quantitative than the models of last resort for the corona that invoke the conversion of magnetic energy as the heating mechanism.
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