http://arxiv.org/abs/2002.07495
This paper is a follow up of the article where Lemaire & Stegen (2016) introduced the novel method to calculate coronal temperature distribution when the Solar Corona is not assumed to be in hydrostatic equilibrium as it has been assumed until 1957. In their study as well as in the present paper it is considered that the corona plasma is expanding with supersonic speeds u_E, and with electron densities n_E, at 1AU is given by the average values determined from the statistical study of the Solar Wind parameters reported by Ebert et al. (2009). In inner coronal altitudes n_e(r) is taken from Saito’s (1970) empirical electron density model. It is found that, at high altitudes, the radial profile of the dyn-temperature distributions differ significantly from those obtained by the scale-height method shm-method generally used in the past. It is also found that, at the base of the Corona, the dyn-temperature is smaller over the polar regions (and CHs) than in the equatorial plane. The temperature gradient dT_e/dr has very small and positive values at altitudes above the transition region, between 0.001 R_S and 0.02 R_S. We confirm also that larger Solar Wind (SW) velocities, u(r), observed in fast speed SW streams imply larger temperatures in the solar Corona. Furthermore, the maximum temperature T_{e,max} is always located significantly above the altitude of the transition region.
J. Lemaire and A. Katsiyannis
Wed, 19 Feb 20
31/62
Comments: 10 pages, 3 figures. Submitted to the Solar Physics journal