On coronal temperatures, temperature gradients and compositions.
Abstract
Average solar wind properties at 1 AU either alone or together with the electron density distribution are used to obtain or review some results that relate coronal temperatures, temperature gradients, and compositions. Measured values of the temperature (T) and the temperature gradient parameter (δ = d ln T/d ln r) are used to find compositions that satisfy the equations used to obtain the results. The total energy equation may be satisfied if the thermal conductivity is reduced by considerable depletions of H^{+} in the corona. The electron energy equation only gives information on coronal compositions that are coupled with dδ/d ln r. The hydrostatic approximation (momentum equation) for the electron density distribution also appears to require considerable depletions of H^{+} in the corona. Results from the integrated momentum equation for the solar wind support the hydrostatic results; together, they give some information on the minimum value of δ in the outer corona. Some changes in assumptions or values of parameters that may modify these interpretations are discussed.
 Publication:

Solar Physics
 Pub Date:
 March 1977
 DOI:
 10.1007/BF00216371
 Bibcode:
 1977SoPh...51..327N
 Keywords:

 Solar Corona;
 Solar Electrons;
 Solar Temperature;
 Solar Wind;
 Electron Density (Concentration);
 Hydrogen Ions;
 Temperature Distribution;
 Thermal Conductivity;
 Wind Measurement;
 Solar Physics;
 Thermal Conductivity;
 Total Energy;
 Temperature Gradient;
 Solar Wind;
 Electron Energy;
 Chemical Composition:Solar Corona;
 Solar Corona:Solar Wind;
 Solar Corona:Temperatures