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Photospheric and “Chromospheric” CIV Lines in B-Main-Sequence Stars

Published online by Cambridge University Press:  04 August 2017

Fiorella Castelli ,
Carlo Morossi  and
Roberto Stalio
Fiorella Castelli
Affiliation:
(*) Osservatorio Astronomico, Trieste
Carlo Morossi
Affiliation:
(*) Osservatorio Astronomico, Trieste
Roberto Stalio
Affiliation:
(**) Dipartimento di Astronomia, University of Trieste

Extract

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The presence in the far-UV spectra of early-type stars of spectral lines of superionized atoms is argument of controversial debate among astronomers. Presently there is agreement on the non-radiative origin of these ions but not on the proposed mechanisms for their production nor on the proposed locations in the stellar atmosphere where they are abundant. Cassinelli et al. (1978) suggest that the Auger mechanism is operative in a cool wind blowing above a narrow corona to produce these ions; Lucy and White (1980) introduce radiative instabilities growing into hot blobs distributed across the stellar wind; Doazan and Thomas (1982) make these ions to be formed in both pre- and post-coronal, high temperature regions at low and high velocity respectively.

Type
Poster Papers - Sessions 1 and 2
Information
Symposium - International Astronomical Union , Volume 116: Luminous Stars and Associations in Galaxies , 1986 , pp. 113 - 116
Copyright
Copyright © Reidel 1986 

References

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Doazan, V., Thomas, R.N.: 1982, in “B-Stars with and without Emission Lines”, ed. Underhill, A.B. and Doazan, V., NASA SP-456 Google Scholar
Doazan, V., Morossi, C., Stalio, R., Thomas, R.N., Willis, A.J.: 1984, Astron. Astrophys., 131, 210.Google Scholar
Doazan, V., Morossi, C., Sedmak, G., Stalio, R., Thomas, R.N.: 1985, Astron. Astrophys., in press.Google Scholar
Lucy, L.B., White, R.L.: 1980, Astrophys. J., 241, 300.CrossRefGoogle Scholar
Molaro, P., Morossi, C., Ramella, M., Franco, M.L.: 1983, Astron. Astrophys., 127, L3.Google Scholar
Underhill, A.B.: 1982, in “B-Stars with and without Emission Lines”, ed. Underhill, A.B. and Doazan, V., NASA SP-456.Google Scholar