Hostname: page-component-848d4c4894-ttngx Total loading time: 0 Render date: 2024-05-08T13:55:29.028Z Has data issue: false hasContentIssue false
  • English
  • Français

A New Class of Wolf-Rayet Stars: WN3/O3s

Published online by Cambridge University Press:  23 January 2015

Philip Massey ,
Kathryn F. Neugent ,
Nidia Morrell  and
D. John Hillier
Philip Massey
Affiliation:
Lowell Observatory email: phil.massey@lowell.edu
Kathryn F. Neugent
Affiliation:
Lowell Observatory email: phil.massey@lowell.edu
Nidia Morrell
Affiliation:
Las Campanas Observatory, Carnegie Observatories
D. John Hillier
Affiliation:
Department of Physics and Astronomy & Pittsburgh Particle Physics, Astrophysics, and Cosmology Center, University of Pittsburgh
Rights & Permissions [Opens in a new window]

Abstract

Core share and HTML view are not available for this content. However, as you have access to this content, a full PDF is available via the ‘Save PDF’ action button.

Our new survey for Wolf-Rayet stars in the Magellanic Clouds is only 15% complete but has already found 9 new Wolf-Rayet (WR) stars in the Large Magellanic Cloud (LMC). This suggests that the total WR population in the LMC may be underestimated by 10-40%. Eight of the nine are of the WN subtype, demonstrating that the “observed” WC to WN ratio is too large, and is biased towards WC stars. The ninth is another rare WO star, the second we have found in the LMC in the past two years. Five (and possibly six) of the 8 WNs are of a new class of WRs, which pose a significant challenge to our understanding. Naively we would classify these stars as “WN3+O3V,” but there are several reasons why such a pairing is unlikely, not the least of which is that the absolute visual magnitudes of these stars are faint, with MV ~ -2.3 to -3.1. We have performed a preliminary analysis with the atmospheric code CMFGEN, and we find that (despite the faint visual magnitudes) the bolometric luminosities of these stars are normal for early-type WNs. Our fitting suggests that these stars are evolved, with significantly enriched N and He. Their effective temperatures are also normal for early-type WNs. What is unusual about these stars is that they have a surprisingly small mass-loss rate compared to other early-type WNs. How these stars got to be the way they are (single star evolution? binary evolution?) remains an open question. For now, we are designating this class as WN3/O3, in analogy to the late-type WN “slash” stars.

Keywords

surveysstars: Wolf-Rayetstars: evolutionstars: early-typegalaxies: individual (LMC)
Type
Contributed Papers
Information
Proceedings of the International Astronomical Union , Volume 9 , Issue S307: New windows on massive stars: asteroseismology, interferometry, and spectropolarimetry , June 2014 , pp. 64 - 69
Copyright
Copyright © International Astronomical Union 2015 

References

Armandroff, T. E. & Massey, P. 1985, ApJ 291, 685CrossRefGoogle Scholar
Bohannan, B. 1990, in Garmany, C. D. (ed.), Properties of Hot Luminous Stars, Vol. 7 of Astronomical Society of the Pacific Conference Series, pp 39–43Google Scholar
Bohannan, B. & Walborn, N. R. 1989, PASP 101, 520CrossRefGoogle Scholar
Breysacher, J., Azzopardi, M., & Testor, G. 1999, A&AS 137, 117Google Scholar
Conti, P. S. 1988, NASA Special Publication 497, 119Google Scholar
Ekström, S., Georgy, C., Eggenberger, P., et al. 2012, A&A 537, A146Google Scholar
Eldridge, J. J., Izzard, R. G., & Tout, C. A. 2008, MNRAS 384, 1109CrossRefGoogle Scholar
Georgy, C., Ekström, S., Eggenberger, P., et al. 2013, A&A 558, A103Google Scholar
Hainich, R., Rühling, U., Todt, H., et al. 2014, A&A 565, A27Google Scholar
Hillier, D. J. & Miller, D. L. 1998, ApJ 496, 407CrossRefGoogle Scholar
Maeder, A., Lequeux, J., & Azzopardi, M. 1980, A&A 90, L17Google Scholar
Massey, P. & Conti, P. S. 1983, ApJ 273, 576CrossRefGoogle Scholar
Massey, P. & Johnson, O. 1998, ApJ 505, 793CrossRefGoogle Scholar
Massey, P., Neugent, K. F., Morrell, N., & Hillier, D. J. 2014, ApJ 788, 83CrossRefGoogle Scholar
Meynet, G., Eggenberger, P., & Maeder, A. 2007, in Vazdekis, A. & Peletier, R. (eds.), Stellar Populations as Building Blocks of Galaxies, Vol. 241 of IAU Symposium, pp 13–22Google Scholar
Meynet, G. & Maeder, A. 2005, A&A 429, 581Google Scholar
Neugent, K. F. & Massey, P. 2011, ApJ 733, 123CrossRefGoogle Scholar
Neugent, K. F., Massey, P., & Georgy, C. 2012a, ApJ 759, 11CrossRefGoogle Scholar
Neugent, K. F., Massey, P., & Morrell, N. 2012b, AJ 144, 162CrossRefGoogle Scholar
Vanbeveren, D. & Conti, P. S. 1980, A&A 88, 230Google Scholar
Walborn, N. R., Sota, A., Maíz Apellániz, J., et al. 2010, ApJ (Letters) 711, L143Google Scholar