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M. Krauss, M. Hanson (University of Cincinnati), R.H.M. Voors (Royal Dutch Meteorological Inst.)
We present high resolution (\lambda/\Delta\lambda ~ 2700) J, H and K band spectroscopy of the Luminous Blue Variable candidate (LBVc) G79.29+0.46* as well as the extensively studied LBVc MWC 349 and prototypical LBV P Cygni. The LBV class is comprised of extremely luminous, evolved stars that have become unstable and undergo periods of significant mass loss. The presence of an HII shell around G79.29+0.46* attests to a relatively recent history of mass loss, with an inferred dynamical age of 2.6\times104 yr (Waters et al. 1996, A&A, 313, 866). Although a large eruption has yet to be observed, it is very likely that G79.29+0.46* is still in the LBV stage, which is thought to last \gtrsim 2.5\times104 yr (Humphreys et al. 1994, PASP, 106, 1025).
We find similarities in the He I (2.058) to H I (Br \gamma) line ratio of G79.29+0.46* and MWC 349 which suggest similar abundances. We also find the spectrum of G79.29+0.46* to be remarkably similar to that of the LBV HR Car (Morris et al. 1997, ASP Conf. Ser. 120). Finally, we note significant spectral variability over the period from 1996 to 1998, especially in the strength of the Mg II 2.137 and 2.144 \mum lines.
The author(s) of this abstract have provided an email address for comments about the abstract: miriam@head-cfa.harvard.edu