000003096 001__ 3096
000003096 005__ 20170202105950.0
000003096 0247_ $$2DOI$$a10.1007/s11207-016-1001-3
000003096 037__ $$aSCART-2017-0023
000003096 100__ $$aLemaire, Joseph
000003096 245__ $$aImproved Determination of the Location of the Temperature Maximum in the Corona
000003096 260__ $$c2016
000003096 520__ $$aThe most used method to calculate the coronal electron temperature [Te (r)] from a coronal density distribution [ne (r)] is the scale-height method (SHM). We introduce a novel method that is a generalization of a method introduced by Alfvén ( Ark. Mat. Astron. Fys. 27, 1, 1941) to calculate Te(r) for a corona in hydrostatic equilibrium: the "HST" method. All of the methods discussed here require given electron-density distributions [ne (r)] which can be derived from white-light (WL) eclipse observations. The new "DYN" method determines the unique solution of Te(r) for which Te(r → ∞) → 0 when the solar corona expands radially as realized in hydrodynamical solar-wind models. The applications of the SHM method and DYN method give comparable distributions for Te(r). Both have a maximum [T_{max}] whose value ranges between 1 - 3 MK. However, the peak of temperature is located at a different altitude in both cases. Close to the Sun where the expansion velocity is subsonic (r < 1.3 R_{⊙}) the DYN method gives the same results as the HST method. The effects of the other free parameters on the DYN temperature distribution are presented in the last part of this study. Our DYN method is a new tool to evaluate the range of altitudes where the heating rate is maximum in the solar corona when the electron-density distribution is obtained from WL coronal observations.
000003096 594__ $$aNO
000003096 6531_ $$aSolar corona
000003096 6531_ $$aCoronal electron temperature
000003096 6531_ $$aSolar wind
000003096 700__ $$aStegen, Koen
000003096 773__ $$c3659-3683$$n12$$pSolar Physics$$v291$$y2016
000003096 8560_ $$fkoen.stegen@observatoire.be
000003096 905__ $$apublished in
000003096 980__ $$aREFERD