Hostname: page-component-78c5997874-4rdpn Total loading time: 0 Render date: 2024-11-19T02:02:40.475Z Has data issue: false hasContentIssue false

Luminous Blue Variables & Mass Loss near the Eddington Limit

Published online by Cambridge University Press:  01 December 2007

Stan Owocki
Affiliation:
Bartol Research Institute, Department of Physics & AstronomyUniversity of Delaware, Newark, DE 19350USA email: [email protected], [email protected]
Allard Jan van Marle
Affiliation:
Bartol Research Institute, Department of Physics & AstronomyUniversity of Delaware, Newark, DE 19350USA email: [email protected], [email protected]
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.

During the course of their evolution, massive stars lose a substantial fraction of their initial mass, both through steady winds and through relatively brief eruptions during their Luminous Blue Variable (LBV) phase. This talk reviews the dynamical driving of this mass loss, contrasting the line-driving of steady winds to the potential role of continuum driving for eruptions during LBV episodes when the star exceeds the Eddington limit. A key theme is to emphasize the inherent limits that self-shadowing places on line-driven mass loss rates, whereas continuum driving can in principle drive mass up to the “photon-tiring” limit, for which the energy to lift the wind becomes equal to the stellar luminosity. We review how the “porosity” of a highly clumped atmosphere can regulate continuum-driven mass loss, but also discuss recent time-dependent simulations of how base mass flux that exceeds the tiring limit can lead to flow stagnation and a complex, time-dependent combination of inflow and outflow regions. A general result is thus that porosity-mediated continuum driving in super-Eddington phases can explain the large, near tiring-limit mass loss inferred for LBV giant eruptions.

Type
Contributed Papers
Copyright
Copyright © International Astronomical Union 2008

References

Belyanin, A. A. 1999, A&A, 344, 199Google Scholar
Castor, J., Abbott, D., & Klein, R. 1975, ApJ, 195, 157 (CAK)CrossRefGoogle Scholar
Gayley, K. 1995, ApJ, 454, 410CrossRefGoogle Scholar
Glatzel, W. 1994, MNRAS, 271, 66.CrossRefGoogle Scholar
Joss, P., Salpeter, E., & Ostriker, J. 1973, ApJ, 181, 429CrossRefGoogle Scholar
Kim, S. S., Figer, D. F., Kudritzki, R. P., & Najarro, F. 2006, ApJ, 653, L113CrossRefGoogle Scholar
Oey, M. S. & Clarke, C. J. 2005, ApJ, 620, L43CrossRefGoogle Scholar
Owocki, S. & Gayley, K. 1997, in: Nota, A. & Lamers, H. (eds.), Luminous Blue Variables: Massive Stars in Transition (San Francisco: ASP), ASP Conf. Ser., 120, 121Google Scholar
Owocki, S., Gayley, K., & Shaviv, N. 2004, ApJ, 558, 802Google Scholar
Quinn, T. & Paczynski, B. 1985, ApJ, 289, 634CrossRefGoogle Scholar
Shaviv, N. 1998, ApJ, 494, L193CrossRefGoogle Scholar
Shaviv, N. 2000, ApJ, 529, L137Google Scholar
Shaviv, N. 2001, ApJ, 549, 1093CrossRefGoogle Scholar
Smith, N. 2002, MNRAS, 337, 1252CrossRefGoogle Scholar
Smith, N., Gehrz, R. D., Hinz, P. M., et al. 2003, AJ, 125, 1458CrossRefGoogle Scholar
Smith, N. & Owocki, S. 2006 ApJ, 645, L45CrossRefGoogle Scholar
Sobolev, V. V. 1960, Moving Envelopes of Stars (Cambridge: Harvard University Press)CrossRefGoogle Scholar
Spiegel, E., & Tao, L. 1999, Phys. Rep. 311, 163CrossRefGoogle Scholar
van Marle, A. J., Owocki, S. P., & Shaviv, N. 2008, in: O'Shea, B., Heger, A. & Abel, T. (eds.), First Stars III, (New York: AIP) in press (arXiv:0708.4207)Google Scholar