By D. De Winter, M. E. Van Den Ancker, M. R. Pérez (auth.), Anne Marie Hubert, Carlos Jaschek (eds.)
The notion of getting a gathering got here to the Editors while engaged on a number of elements of galactic Be and B[e] stars. they discovered normal precis of the homes of B[e] stars used to be lacking, in order that the organiza tion of a primary assembly on those items seemed as very beneficial. B[e] stars have hydrogen line emission and forbidden [Fe eleven] and [0 I] emission strains of their spectra; also they are characterised through a powerful IR extra because of circumstellar dirt. Having a large number of extinction within the UV and the visible they've been much less usually saw than different emission line items. even though approximately 100 galactic items were categorised as B[e], in basic terms fif teenager or so were studied in a few aspect. along with this, the evolutionary prestige of those gadgets is rat her arguable, are they pre-main series or stars which will turn into nUclei of planetary nebulae? different tough difficulties look while contemplating the kin of those stars with different related teams, like Herbig AeBe stars, Be, luminous blue variables and the superluminous B[e] stars saw within the Magellanic Clouds. The convention turns out well timed considering that huge surveys like DENIS and 2Mass, plus new house and new tools for the micron, millimeter and cen timeter wavelength area will bring about the invention of extra stars of this group.
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Additional info for B[e] Stars: Proceedings of the Paris Workshop held from 9–12 June, 1997
The abbreviations in the heading refer to the original studies: dW = de Winter et al. (1997); Hil = Hillenbrand et al. (1993); MP = Perez et al. (1987, 1991); PT2 = TM et al. (1985); PT2 = The et al. (1990); vdA = van den Ancker et al. (1997). For some cluster properties estimates are given with the error between parentheses. 3 0 6611 6611 Total dW+PT2 Hil Notes: *) Taken from Luiken-Miller (1982). **) Taken from Sagar & Joshi (1978). ) survival time is ~107 yrs. The latter is supported by the detection of Hester et al.
Like in this study, we have only low resolution spectroscopy. It is evident that high resolution spectra is needed to resolve indications of accretion, such as inversed P Cygni profiles, such as has been detected for several Herbig Ae/Be stars in Ha. Lamers: You find that the dusty-disk of HAeBe stars can disappear due to erosion by hot stars in the same cluster. But why don't you see forbidden emission lines? Is the presence of dust a necessary condition for the formation of [e] lines? de Winter: This seems to be proven observationally.
98, D. Reidel, Dordrecht, p. , 1990. In: Evolution in Astrophysics, Proc. Int. , Toulouse, ESA SP-310, p. , Shepherd D. et al. , 1994. In: The Nature and Evolutionary Status of Herbig Ae/Be Stars, eds. J. van den Heuvel, ASP Conference Sero Vol. 62, p. , Pottasch S. H. , 1989. In: Physics of Luminous BIue Variables, eds. K. J. M. Lamers, Kluwer Academic Publishers, Dordrecht, p. , 1996. In: Light curves of variable stars, eds. C. Sterken and C. R, 1970, Mem. R astr. Soc. , 1997. In: Luminous BIue Variables: Massive Stars in Transition; eds.