High-Resolution J, H and K Band Spectroscopy of the Luminous Blue Variable Candidate in G79.29+0.46

Details High-Resolution J, H and K Band Spectroscopy of the Luminous Blue Variable Candidate in G79.29+0.46 High-Resolution J, H and K Band Spectroscopy of the Luminous Blue Variable Candidate in G79.29+0.46

Dec 2000

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2000aas...197.4412k&link_type=abstract

American Astronomical Society, 197th AAS Meeting, #44.12; Bulletin of the American Astronomical Society, Vol. 32, p.1473

Astronomy and Astrophysics

Astronomy

Scientific paper

We present high resolution (λ /Δ λ ~ 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 2.6x104 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 ≳ 2.5x104 yr (Humphreys et al. 1994, PASP, 106, 1025). We find similarities in the He I (2.058) to H I (Br γ ) 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 μ m lines.

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