Hostname: page-component-76fb5796d-qxdb6 Total loading time: 0 Render date: 2024-04-25T11:08:32.761Z Has data issue: false hasContentIssue false
  • English
  • Français

What Do We Really Know About the Winds of Massive Stars?

Published online by Cambridge University Press:  01 December 2007

D. John Hillier
D. John Hillier*
Affiliation:
Department of Physics & Astronomy, University of Pittsburgh, 3941 O'Hara Street, Pittsburgh, PA, 15260, USA email: hillier@pitt.edu
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.

The standard theory of radiation driven winds has provided a useful framework to understand stellar winds arising from massive stars (O stars, Wolf-Rayet stars, and luminous blue variables). However, with new diagnostics, and advances in spectral modeling, deficiencies in our understanding of stellar winds have been thrust to the forefront of our research efforts. Spectroscopic observations and analyses have shown the importance of inhomogeneities in stellar winds, and revealed that there are fundamental discrepancies between predicted and theoretical mass-loss rates. For late O stars, spectroscopic analyses derive mass-loss rates significantly lower than predicted. For all O stars, observed X-ray fluxes are difficult to reproduce using standard shock theory, while observed X-ray profiles indicate lower mass-loss rates, the potential importance of porosity effects, and an origin surprisingly close to the stellar photosphere. In O stars with weak winds, X-rays play a crucial role in determining the ionization balance, and must be taken into account.

Keywords

stars: atmospheres – stars: mass loss – stars: windsoutflows – stars: individual (10 Lac, τ Sco, ζ Pup) – stars: early-type – line: formation – line: profiles
Type
Contributed Papers
Information
Proceedings of the International Astronomical Union , Volume 3 , Symposium S250: Massive Stars as Cosmic Engines , December 2007 , pp. 89 - 96
Copyright
Copyright © International Astronomical Union 2008

References

Allen, C. W. 1973, Astrophysical Quantities, 3rd. ed. (London: University of London, Athlone Press)Google Scholar
Asplund, M., Nordlund, Å., Trampedach, R., et al. 2000, A&A, 359, 729Google Scholar
Berghöfer, T. W., Schmitt, J. H. M. M., & Cassinelli, J. P. 1996, A&AS, 118, 481Google Scholar
Bouret, J.-C., Lanz, T., Hillier, D. J., & Foellmi, C. 2008a, in: Hamann, W.-R., Feldmeier, A., Oskinova, L. M. (eds.), Clumping in Hot Star Winds (Potsdam: Universitäts-Verlag), in pressGoogle Scholar
Bouret, J.-C., Lanz, T., Hillier, D. J., & Foellmi, C. 2008b, in preparationGoogle Scholar
Bouret, J.-C., Lanz, T., Hillier, D. J., Heap, S. R., et al. 2003, ApJ, 595, 1182Google Scholar
Busche, J. R. & Hillier, D. J. 2005, AJ, 129, 454Google Scholar
Castor, J. I., Abbott, D. C., & Klein, R. I. 1975, ApJ, 195, 157Google Scholar
Cohen, D. H., de Messières, G. E., MacFarlane, J. J., et al. 2003, ApJ, 586, 495Google Scholar
Cox, A. N. 2000, in: Cox, A. N. (ed.), Allen's Astrophysical Quantities, 4th ed. (New York: AIP Press; Springer)Google Scholar
Crowther, P. A., Hillier, D. J., Evans, C. J., et al. 2002, ApJ, 579, 774Google Scholar
Donati, J.-F., Howarth, I. D., Jardine, M. M., et al. 2006, MNRAS, 370, 629Google Scholar
Eversberg, T., Lepine, S., & Moffat, A. F. J. 1998, ApJ, 494, 799Google Scholar
Feldmeier, A., Puls, J., & Pauldrach, A. W. A. 1997, A&A, 322, 878Google Scholar
Hillier, D. J. 1991, A&A, 247, 455Google Scholar
Hillier, D. J. 2003, in: Hucht, K. van der, Herrero, A., & Esteban, C. (eds.), A Massive Star Odyssey: From Main Sequence to Supernova (San Francisco: ASP), Proc. IAU Symp 212, 70Google Scholar
Hillier, D. J., Lanz, T., Heap, S. R., et al. 2003, ApJ, 588, 1039Google Scholar
Hillier, D. J. & Miller, D. L. 1998, ApJ, 496, 407Google Scholar
Hubeny, I. & Lanz, T. 1995, ApJ, 439, 875Google Scholar
Kaufer, A., Stahl, O., & Prinja, R. K. 2007, in: Okazaki, A. T., Owocki, S. P., & Stefl, S. (eds.), Active OB-Stars: Laboratories for Stellar and Circumstellar Physics (San Francisco: ASP), ASP Conf. Ser., 361, 179Google Scholar
Kaufer, A., Stahl, O., Wolf, B., et al. 1997, A&A, 320, 273Google Scholar
Kramer, R. H., Cohen, D. H. & Owocki, S. P. 2003, ApJ, 592, 532Google Scholar
Lamers, H. J. G. L. M. & Cassinelli, J. P. 1999, Introduction to Stellar Winds (Cambridge: Cambridge University Press)Google Scholar
Lamers, H. J. G. L. M. & Rogerson, J. B. Jr., 1978, A&A, 66, 417Google Scholar
Lanz, T., Hillier, D. J., Hubeny, I. J., et al. 2008, in preparationGoogle Scholar
Lépine, S. & Moffat, A. F. J. 1999, ApJ, 514, 909CrossRefGoogle Scholar
Lucy, L. B. 2007a, A&A, 468, 649Google Scholar
Lucy, L. B. 2007b, A&A, 474, 701Google Scholar
Lucy, L. B. & Solomon, P. M. 1970, ApJ, 159, 879Google Scholar
Lucy, L. B. & White, R. L. 1980, ApJ, 241, 300Google Scholar
Maeder, A., Georgy, C., & Meynet, G. 2008, 479, L37Google Scholar
Markova, N., Puls, J., Repolust, T., & Markov, H. 2004, A&A, 413, 693Google Scholar
Martins, F., Schaerer, D., Hillier, D. J., & Heydari-Malayeri, M. 2004, A&A, 420, 1087Google Scholar
Martins, F., Schaerer, D., Hillier, D. J., et al. 2005, A&A, 441, 735Google Scholar
Mokiem, M. R., de Koter, A., Evans, C. J., et al. 2007, A&A, 465, 1003Google Scholar
Mokiem, M. R., de Koter, A., Puls, J., et al. 2005, A&A, 441, 711Google Scholar
Oskinova, L. M., Feldmeier, A., & Hamann, W.-R. 2006, MNRAS, 372, 313Google Scholar
Oskinova, L. M., Hamann, W.-R., & Feldmeier, A. 2007, A&A, 476, 1331Google Scholar
Owocki, S. P. 2008, in: Hamann, W.-R., Feldmeier, A., Oskinova, L. M. (eds.), Clumping in Hot Star Winds (Potsdam: Universitäts-Verlag), in pressGoogle Scholar
Owocki, S. P. & Cohen, D. H. 2006, ApJ, 648, 565Google Scholar
Owocki, S. P., & ud-Doula, A. 2004, ApJ, 600, 1004Google Scholar
Owocki, S. P. & Puls, J. 1999, ApJ, 510, 355Google Scholar
Owocki, S. P., Castor, J. I., & Rybicki, G. B. 1988, ApJ, 335, 914Google Scholar
Pauldrach, A. W. A., Kudritzki, R. P., Puls, J., & Butler, K. 1990, A&A, 228, 125Google Scholar
Petrenz, P. & Puls, J. 1996, A&A, 312, 195Google Scholar
Petrenz, P. & Puls, J. 2000, A&A, 358, 956Google Scholar
Poe, C. H., Owocki, S. P., & Castor, J. I. 1990, ApJ, 358, 199Google Scholar
Puls, J., Markova, N., Scuderi, S., et al. 2006, A&A, 454, 625Google Scholar
Sana, H., Rauw, G., Nazé, Y., et al. 2006, MNRAS, 372, 661Google Scholar
Shaviv, N. J. 2001, ApJ, 549, 1093Google Scholar
Simón-Díaz, S. & Herrero, A. 2007, A&A, 468, 1063Google Scholar
Stothers, R. B. 2003, ApJ, 589, 960CrossRefGoogle Scholar
Vink, J. S., de Koter, A., & Lamers, H. J.G. L.M. 2000, A&A, 362, 295Google Scholar
Walborn, N. R., Lennon, D. J., Heap, S. R., et al. 2000, PASP 112, 1243Google Scholar