Formation of OI resonance triplet lines in the solar spectrum

Journal Article · Tue Mar 01 04:00:00 EST 1977 · Sov. Astron. AJ (Engl. Transl.); (United States)

OSTI ID:7281868

Nagirner, D I; Shneivais, A B

The OI emission resonance triplet (1302, 1304, 1306 A) in the solar spectrum is studied on the basis of the theory of the formation of a resonance multiplet. It is assumed that the population distribution of atoms over the sublevels of the lower (ground) state is a Boltzmann distribution, scattering is conservative and takes place with complete frequency redistribution of the radiation within each line, the coefficients of absorption in the lines are Doppler coefficients, and the atmosphere is semiinfinite. Using an H-function calculated earlier for primary sources which decrease exponentially with depth, profiles of the triplet lines are constructed and the total intensities and fluxes are found. A comparison with calculations for rectangular line profiles showed that the frequency redistribution is important. The results are in satisfactory agreement with observations.

• Research Organization: Astronomical Observatory of Leningrad State University
• OSTI ID: 7281868
• Journal Information: Sov. Astron. AJ (Engl. Transl.); (United States), Journal Name: Sov. Astron. AJ (Engl. Transl.); (United States) Vol. 21:2; ISSN SAAJA
• Country of Publication: United States
• Language: English

Related Subjects

640104* -- Astrophysics & Cosmology-- Solar Phenomena
71 CLASSICAL AND QUANTUM MECHANICS
GENERAL PHYSICS
ATMOSPHERES
DOPPLER BROADENING
EMISSION SPECTRA
ENERGY SPECTRA
ENERGY-LEVEL TRANSITIONS
FUNCTIONS
LINE BROADENING
LINE WIDTHS
MATHEMATICAL MODELS
RADIATIONS
SOLAR ATMOSPHERE
SOLAR RADIATION
SPECTRA
SPECTRAL FUNCTIONS
STAR MODELS
STARS
SUN