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Infrared emission lines of Mg II in B stars

  • T. A. Aaron Sigut (a1) and J. B. Lester (a1)

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Recently, Chang et. al. (1992) and Carlsson, Rutten and Shchukina (1992) (CRS) demonstrated the non-LTE formation mechanism behind the 12 μm Mg I emission lines (6g–7h, 6h–7i) observed in the solar spectrum (Murcray et. al., 1981). CRS stress the generality of this mechanism showing that it is a natural consequence of the recombination flow from the large Mg II reservoir through the Rydberg levels of Mg I. We have noted the close parallel between Mg I in the solar atmosphere and Mg II in the atmospheres of B stars (where Mg III plays the role of the reservoir) and investigated the operation of this mechanism in high-ℓ infrared transitions of Mg II. We have employed a 58 level Mg II atom including all energy levels through n = 25 and a total of 491 linearized radiative transitions. The coupled equations of radiative transfer and statistical equilibrium were solved with the MULTI code in its local operator form (Carlsson, 1992).

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References

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Carlsson, M., Rutten, R.J., Shchukina, N.G.: 1991, Astr. Ap. 253, 567
Carlsson, M.: 1992, ‘The MULTI non-LTE program’ in Giampapa, M. S. and Bookbinder, J. A., ed(s)., Cool Stars, Stellar Systems and the Sun , A.S.P. Conf. Ser. Vol. 26, 499
Chang, E.S., Avrett, E.H., Mauas, P.J., Noyes, R.W., Loeser, R.: 1991, Ap. J.(Letters) 379, L79
Collins, G.W.: 1963, Ap. J. 138, 1134
Murcray, F.J., Goldman, A., Murcray, F.H., Bradford, C.M., Murcray, D.G., Coffey, M.T., Mankin, W.G.: 1981, Ap. J.(Letters) 247, L97

Infrared emission lines of Mg II in B stars

  • T. A. Aaron Sigut (a1) and J. B. Lester (a1)

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