Improving the Ni I atomic model for solar and stellar atmospheric models
Abstract
Neutral nickel (Ni I) is abundant in the solar atmosphere and is one of the important elements that contribute to the emission and absorption of radiation in the spectral range between 1900 and 3900 A. Previously, the Solar Radiation Physical Modeling (SRPM) models of the solar atmosphere considered only few levels of this species. Here we improve the Ni I atomic model by taking into account 61 levels and 490 spectral lines. We compute the populations of these levels in full NLTE using the SRPM code and compare the resulting emerging spectrum with observations. The present atomic model improves significantly the calculation of the solar spectral irradiance at near-UV wavelengths that are important for Earth atmo spheric studies, and particularly for ozone chemistry.
Cite
@article{arxiv.1303.3528,
title = {Improving the Ni I atomic model for solar and stellar atmospheric models},
author = {Mariela C. Vieytes and Juan M. Fontenla},
journal= {arXiv preprint arXiv:1303.3528},
year = {2015}
}
Comments
Accepted for publication in The Astrophysical Journal