Remaining Line Opacity Problems for the Solar Spectrum

Details Remaining Line Opacity Problems for the Solar Spectrum Remaining Line Opacity Problems for the Solar Spectrum

Mar 1992

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1992rmxaa..23..187k&link_type=abstract

Revista Mexicana de Astronomia y Astrofisica, 23, 187

Astronomy and Astrophysics

Astrophysics

55

Scientific paper

RESUMEN. Se necesita tener espectros solares de ata resoluci6n y alta seflal a ruido con cobertura espectral completa. El espectro solar provee la energia que controla la qufmica atmosf6rica de la Lierra y del resto de los cuerpos del sistema solar. Es importante para Ia astroffsica estelar porque constituye el espectro estelar "estandar", ya. que puede ser observado mejor que el de cualquier otra estrella. Es importante para comprender al sol, ya que permite estudiar las condiciones y los movimientos en 511 superficie. Constituye Un importante laboratorio de altas temperaturas para la espectroscopfa at6mica y mde'cular. Para interpretar este espectro se requiere tener conocimiento preciso sobre los niveles de energfa, longitudes de onda, valores gf y constantes de amortiguamiento. Se requiere conocer los desdoblamientos hiperfino, isot6pico y Zeeman. Se requiere completitud para deconvolucionar las confusiones de lfneas espectrales. Se requiere conocer cada nivel que este' por debajo de la primera energfa de ionizadon 0 disociaci6n. Para las mol6culas, esto significa conocer cada nivel vibracional y rotacional. ABSTRACT. We need high-resolution, high-signal-to-noise spectra of the sun with complete spectral coverage. The solar spectrum provides the insolation that controls the atmospheric chemistry of the earth and of all the solar system bodies. It is important for stellar astrophysics as the "standard" stellar spectrum because it can be observed better than that of any other star. It is important for understanding the sun, for it allows us to study the conditions and motions at its surface. It is an important high-temperature laboratory source for atomic and molecular spectroscopy. To interpret the spectrum we require accurate energy levels, accurate wavelengths, accurate gf values, accurate damping constants. We require hyperfine splitting, isotopic splitting, and Zeeman splitting. We require completeness in order to deconvolve blends. We need every level below the lowest ionization or dissociation energy. For molecules that is every vibrational and rotational level. Key words: ATOMIC PROCESSES - MOLECULAR PROCESSES - TRANSITION PROBABILITIES - SUN: SPECTRA

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