Las líneas del Si I como diagnóstico de la estructura de la atmósfera solar

CINCUNEGUI, C. C.; LUONI, M.L.; MAUAS, P J D

Congreso; reunión Anual de la Asociación Argentina de Astronomía; 1998

Asociación Argentina de Astronomía

The H and K lines of Ca II, λ3933.66 Å and λ3968.47 Å respectively, are between the most studied spectral lines, both in the solar and in the stellar cases. This is due to the special sensitive to the activity levels and the amount of information that they give about the cromospheric structure. In particular, the blue light spectrographer (BLISP) which will be soon placed in the CASLEO Observatory in San Juan will observe the sun in that zone of the spectrum. Therefore, it is very important to find other atomic lines in the same spectral region than can complement the information given by the calcium lines. One of the broadest lines found in this zone is the Si I λ3905.52 Å. In this work we present a model of neutral silicon which consist of 21 levels. It was used to calculate the profile of λ3905.52 Å for the quiet Sun model of Vernazza, Avrett and Loeser (1981, ApJS 45, 635) using the Pandora program, wich selfconsistently solves the transport and statistical equilibrium equations. We also calculate the profile of λ4102.94 Å, a line very close to Hδ (λ4101.7 Å), to confirm the model. The agreement between the observed and computed profiles is very good.