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The Ni I lines in the solar spectrum

Published online by Cambridge University Press:  05 July 2012

Mariela C. Vieytes ,
Pablo J. D. Mauas  and
Juan M. Fontenla
Mariela C. Vieytes
Affiliation:
Instituto de Astronomía y Física del Espacio Universidad Nacional de Tres de Febrero, email: mariela@iafe.uba.ar
Pablo J. D. Mauas
Affiliation:
Instituto de Astronomía y Física del Espacio Universidad de Buenos Aires, Buenos Aires, Argentina email: pablo@iafe.uba.ar
Juan M. Fontenla
Affiliation:
Laboratory for Atmospheric and Space Physics, University of Colorado, Boulder, USA email: juan.fontenla@lasp.colorado.edu
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Abstract

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The stratosphere is the region where the ozone chemistry is important for the balance of energy, and radiation in the near UV plays a fundamental role in the creation and destruction of ozone. However, the radiation in this range of wavelength has not been very well modeled. One of the most important elements, according to its abundance in the solar atmosphere, that contribute to the emission and absorption of radiation in the spectral range between 1900 and 3900 Å, is neutral nickel (Ni I). In this work we improve the atomic model of this element, taking into account 490 lines over the spectrum. We solve these lines in NLTE using the Solar Radiation Physical Modeling (SRPM) program and compare the results with observation of the quiet sun spectrum.

Keywords

radiative transferline: profilesSun: spectral irradiance
Type
Contributed Papers
Information
Proceedings of the International Astronomical Union , Volume 7 , Symposium S286: Comparative Magnetic Minima: Characterizing quiet times in the Sun and Stars , October 2011 , pp. 93 - 96
Copyright
Copyright © International Astronomical Union 2012

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