Flow properties of the solar wind obtained from white light data and a two-fluid modelThe flow properties of the solar wind from 1 R(sub s) to 1 AU were obtained using a two fluid model constrained by density and scale height temperatures derived from white light observations, as well as knowledge of the electron temperature in coronal holes. The observations were obtained with the white light coronographs on SPARTAN 201-1 and at Mauna Loa (Hawaii), in a north polar coronal hole from 1.16 to 5.5 R(sub s) on 11 Apr. 1993. By specifying the density, temperature, Alfven wave velocity amplitude and heating function at the coronal base, it was found that the model parameters fit well the constraints of the empirical density profiles and temperatures. The optimal range of the input parameters was found to yield a higher proton temperature than electron temperature in the inner corona. The results indicate that no preferential heating of the protons at larger distances is needed to produce higher proton than electron temperatures at 1 AU, as observed in the high speed solar wind.
Document ID
19950025483
Acquisition Source
Legacy CDMS
Document Type
Conference Paper
Authors
Habbal, Shadia Rifai (Harvard-Smithsonian Center for Astrophysics Cambridge, MA., United States)
Esser, Ruth (Harvard-Smithsonian Center for Astrophysics Cambridge, MA., United States)
Guhathakurta, Madhulika (NASA Goddard Space Flight Center Greenbelt, MD, United States)
Fisher, Richard (NASA Goddard Space Flight Center Greenbelt, MD, United States)
Date Acquired
August 16, 2013
Publication Date
December 1, 1994
Publication Information
Publication: ESA, Proceedings of 3rd SOHO Workshop on Solar Dynamic Phenomena and Solar Wind Consequences