ANALYSIS OF THE HYDROGEN ECLIPSE OBSERVATIONS TO DETERMINE THE THERMODYNAMIC STATE OF THE SOLAR CHROMOSPHERE
Abstract
An attempt is made to investigate features of the hydrogen spectrum which may be unambiguously interpreted to specify certain gross features of the structure of the chromosphere. A theoretical analysis of the data to be obtained at the 1952 eclipse is given. Resolution of the dilemma between radio and optical observations of the outer solar atmosphere is desired. On the basis of thermodynamic equilibrium and an atmosphere transparent to its own radiation, the computed Balmer decrement is in every case to high. Departures from thermodynamic equilibrium are included by introducing the standard b sub n which is defined so as to help give agreement between the theoretical and observed Balmer decrement. Self-absorption effects are also included, and no attempt is made to specify the electron temperature Tau sub epsilon. From a comparison of 2 methods of estimating the hydrogen density gradient, a demonstration of the direction of deviation of the chromosphere from thermodynamic equilibrium is obtained in which b sub n > b sub n+k > 1, where the subscripts refer to the quantum numbers. The application of the proposed methods to the reduction of the 1952 eclipse data should provide values of Nu , Tau sub epsilon, Delta Tau sub epsilon and Delta Nu sub epsilon at a number of heights in the atmosphere.
Document Details
- Document Type
- Technical Report
- Publication Date
- Jul 17, 1952
- Accession Number
- AD0001761
Entities
People
- Eugene N. Parker
- Richard N. Thomas
Organizations
- High Altitude Observatory