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On the coronal lines λ5303 Å and λ6374 Å

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Abstract

We present theoretical calculations of the observed coronal emission line profiles of Fexiv (5303 Å) and Fex (6374 Å) ions, which are observed at the time of total solar eclipse. Baumbach's relation (Allen, 1973) of electron density has been employed to compute the full width at half maximum FWHM. We have employed several other electron density distributions and found that the calculated differences in the FWHM are within 0.5% of one another. We have used the ion densities N i/NE given by Jordan (1969). To explain the observed FWHM, we have assumed that the corona is expanding spherically symmetrically with a velocity of one or two mean thermal units and no turbulence is included. With these highly simplified assumptions, we have reproduced qualitatively the profiles and FWHM's of the above lines. However, to explain quantities of FWHM's, we should take into account the inhomogeneities in the structure of the corona. It is thus shown, that turbulence is not necessary to explain the observed FWHM.

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  1. Indian Institute of Astrophysics, 560 034, Bangalore, India

    A. Peraiah & B. A. Varghese

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  1. A. Peraiah
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  2. B. A. Varghese
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Peraiah, A., Varghese, B.A. On the coronal lines λ5303 Å and λ6374 Å. Sol Phys 124, 53–72 (1989). https://doi.org/10.1007/BF00146519

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  • DOI: https://doi.org/10.1007/BF00146519

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