Synthesis of several solar hydrogen lines

Details Synthesis of several solar hydrogen lines Synthesis of several solar hydrogen lines

Apr 1976

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1976a%26a....48...75z&link_type=abstract

Astronomy and Astrophysics, vol. 48, no. 1, Apr. 1976, p. 75-82.

Astronomy and Astrophysics

Astrophysics

2

H Lines, Line Spectra, Solar Spectra, Spectrum Analysis, Stark Effect, Absorptivity, Graphs (Charts), H Alpha Line, H Beta Line, H Gamma Line, Hydrogen Atoms, Photoionization, Thermodynamic Equilibrium

Scientific paper

A model hydrogen atom consisting of five bound levels plus continuum is used along with the Harvard Smithsonian Reference Atmosphere to synthesize the solar H-alpha, H-beta, H-gamma, P-alpha, P-beta, and B-alpha lines under the assumption of kinetic equilibrium. The P-alpha, P-beta, and B-alpha lines are also calculated under the assumption of local thermodynamic equilibrium. Photoionization rates are computed by numerical integration over all pertinent frequencies, the line absorption coefficients employed are identified, and the resulting profiles of the emitted radiation are plotted. It is found that: (1) extension of the model atom to five bound levels leads to an intensity increase of 20% for the H-alpha line center in comparison with the three-level model; (2) the H-alpha and H-beta cores are too narrow and too deep; (3) the H-beta, H-gamma, and B-alpha wings are slightly too bright; and (4) the calculated profiles lie within the limits of observational error for the non-LTE H-gamma line core, the non-LTE P-alpha line, and the LTE P-beta line. The discrepancies are attributed to errors in the absorption coefficients, the photoionization rates, and the atmospheric model.

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