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THE SOLAR Mg II h AND k LINES – Observations and Radiative Transfer Modeling

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Abstract

This paper presents observations of the MgII h and k lines obtained with the UVSP instrument that flew aboard the SMM satellite. Both spatially averaged and resolved observations are compared with calculated profiles of the lines from standard, plane-parallel solar models. The radiative transfer calculations presented take full account of partial frequency redistribution and wavelength overlap of the h and k lines. A comparison between theoretical and observed wing profiles indicates that current one-dimensional models underestimate the temperature in the middle photosphere. The cores of spatially resolved dark intra-network profiles are well reproduced by the model calculations, while the spatially averaged profiles have in general broader emission peaks, indicating that the additional broadening is due to a contribution of magnetic network profiles.

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  1. Harvard–Smithsonian Center for Astrophysics, 60 Garden St., Cambridge, MA, 02138, U.S.A.

    H. Uitenbroek

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  1. H. Uitenbroek
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Uitenbroek, H. THE SOLAR Mg II h AND k LINES – Observations and Radiative Transfer Modeling. Solar Physics 172, 109–116 (1997). https://doi.org/10.1023/A:1004981412889

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  • DOI: https://doi.org/10.1023/A:1004981412889

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