The consequences are presented of a postulated nonthermal distribution at the point in a stellar atmosphere where the plasma is nearly fully ionized and optically thin. The most immediate consequences are (1) that the temperature and quasi-neutral plasma density become anticorrelated with increasing radius in a thin transition region, leaving the temperature profile inverted in excess of 10(6) K up into a corona without depositing wave or magnetic field energy into the gas above the base of the transition region as suggested to be possible in the previous paper (Scudder 1992a, hereafter Paper I); (2) that the temperature inversion process is essentially independent of magnetic topology working only slightly more efficiently on "closed" than on "open" flux tubes; (3) that the inversion temperature scale height can be extremely short for stars on the main sequence; (4) that there is an alternative suprathermal interpretation for the excess or "turbulent" Doppler widths by generalizing the Voigt-Hjerting line profile; (5) that the observed temperature dependence of the excess UV Doppler widths can be derived; (6) that a determination of a measure, kappa+(-1), of the ion nonthermal tail strength in the solar transition region of kappa+ = 2.2 +/- 0.8 implies a transition region temperature scale height of congruent-to 400 km, consistent with observations (for reference kappa = infinity is a Gaussian); (7) that a transition region/low coronal temperature profile from the inferred value of kappa simply produces solar coronal temperatures as a direct generalization of the exponential atmosphere; (8) that there is more than enough energy flux to sustain the solar corona against its known losses for 2.49 < kappa < 6.25; (9) that various correlations of heating with magnetic orientation and altitude in loops and sunspots follow as ready corollaries of this postulate; (10) that inversion temperatures in excess of 10(6) K for representative ZAMS stars are obtained, suggesting that they are capable of thermal X-ray emission as observed; (I 1) that the Parker critical point location in stellar radii is proportional to kappa and always above the stellar surface; (12) that the asymptotic wind speeds scale as U(infinity) congruent-to O(1)V(esc)/kappa1/2; (13) that U(infinity)(1 AU) at Earth is estimated to be between 300 and 600 km s-1, consistent with kappa-values in the range 2.4-7.1; (14) that values of kappa determined for different groups of stars based on the scaling of item (12) determine credible maximum inversion temperatures for these groups, including an explanation of why some classes of stars usually are not X-ray emitters; and (15) that a mechanism exists for "heating" solar wind minor ions proportionally to their mass.
