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The Variable Shell Star HR 5999

Published online by Cambridge University Press:  12 April 2016

P.S. Thé  and
H.R.E. Tjin A Djie
P.S. Thé
Affiliation:
Astronomical Institute, University of Amsterdam, Roetersstraat 15, 1018 WB Amsterdam, The Netherlands
H.R.E. Tjin A Djie
Affiliation:
Astronomical Institute, University of Amsterdam, Roetersstraat 15, 1018 WB Amsterdam, The Netherlands

Extract

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From spectroscopic observations Bessell and Eggen (1972) (hereafter called BE) have detected that HR 5999 (erroneously named HR 6000 by BE) is a shell star of spectral type A7 III-IV with hydrogen lines in emission. Photometric observations show subsequently that HR 5999 varies in brightness up to about 1 mag semiregularly with a period of about 1 month. Eggen (1975) believes that HR 5999 forms a pre-main sequence object.

With HR 6000, the star HR 5999 forms a visual double star system named Δ199; HR 5999 is the southern component. The angular separation is about 45”. BE show that these stars have a common proper motion, and are, therefore, believed to form a physical pair.

Type
Part I: Young Objects
Information
International Astronomical Union Colloquium , Volume 42: The Interaction of Variable Stars with their Environment , 1977 , pp. 137 - 143
Copyright
Copyright © Veröff. Der Remeis-Sterwarte 1977

References

Bessell, M.S., Eggen, O.J.: 1972, Astroph. J. 177, 209.CrossRefGoogle Scholar
Eggen, O.J.: 1975, Publ. Astron. Soc. Pacific 87, 37.Google Scholar
Larson, R.B.: 1972, Monthly Notices Roy. Astron. Soc. 157, 121.Google Scholar
Lub, J., Pel, J.W.: 1977, Astron. Astroph. 54, 137.Google Scholar
Rijf, R., Tinbergen, J., Walraven, Th.: 1969, Bull. Astron. Inst. Neth., 20, 279.Google Scholar
Thé, P.S.: 1962, Contrib. Bosscha Obs. No. 15.Google Scholar
Walraven, Th., Walraven, J.H.: 1960, Bull. Astron. Inst. Neth. 15, 67.Google Scholar