Hostname: page-component-6bf8c574d5-w79xw Total loading time: 0 Render date: 2025-02-17T01:57:52.904Z Has data issue: false hasContentIssue false
  • English
  • Français

Mass loss and fate of the most massive stars

Published online by Cambridge University Press:  05 September 2012

Jorick S. Vink
Jorick S. Vink*
Affiliation:
Armagh Observatory, College Hill, BT61 9DG, Armagh, United Kingdom email: [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.

The fate of massive stars up to 300M⊙ is highly uncertain. Do these objects produce pair-instability explosions, or normal Type Ic supernovae? In order to address these questions, we need to know their mass-loss rates during their lives. Here we present mass-loss predictions for very massive stars (VMS) in the range of 60-300M⊙. We use a novel method that simultaneously predicts the wind terminal velocities v∞ and mass-loss rate Ṁ as a function of the stellar parameters: (i) luminosity/mass Γ, (ii) metallicity Z, and (iii) effective temperature Teff. Using our results, we evaluate the likely outcomes for the most massive stars.

Keywords

stars: mass lossstars: evolutionstars: Wolf-Rayetsupernovae: general
Type
Contributed Papers
Information
Proceedings of the International Astronomical Union , Volume 7 , Symposium S279: Death of Massive Stars: Supernovae and Gamma-Ray Bursts , April 2011 , pp. 29 - 33
Copyright
Copyright © International Astronomical Union 2012

References

Bestenlehner, J. M., Vink, J. S., Gräfener, G., et al. , 2011, A&A 530L, 14Google Scholar
Castor, J. I., Abbott, D. C., & Klein, R. I., 1975, ApJ 195, 157CrossRefGoogle Scholar
Crowther, P. A., Schnurr, O., Hirschi, R., et al. , 2010, MNRAS 408, 731CrossRefGoogle Scholar
Eldridge, J. J. & Vink, J. S., 2006, A&A 452, 295Google Scholar
Evans, C. J., Taylor, W. D., Henault-Brunet, V., et al. 2011, A&A 530, 108Google Scholar
Gräfener, G. & Hamann, W.-R. 2008, A&A 482, 945Google Scholar
Gräfener, G., Vink, J. S., de Koter, A., & Langer, N., 2011, A&A 535, 56Google Scholar
Gräfener, G., Owocki, S. P., & Vink, J. S., 2012a, A&A 538, 40Google Scholar
Groh, J. H. & Vink, J. S., 2011, A&A 531L, 10Google Scholar
Heger, A., Fryer, C. L., Woosley, S. E., et al. , 2003, ApJ 591, 288CrossRefGoogle Scholar
Ishii, M., Ueno, M., & Kato, M., 1999, PASJ 51, 417CrossRefGoogle Scholar
Kotak, R. & Vink, J. S., 2006, A&A 460L, 5Google Scholar
Muijres, L., Vink, J. S., de Koter, A., et al. , 2012, A&A 537, 37Google Scholar
Müller, P. E. & Vink, J. S., 2008, A&A 492, 493Google Scholar
Nugis, T., & Lamers, H. J. G. L. M., 2002, A&A 389, 162Google Scholar
Trundle, C., Kotak, R., Vink, J. S., & Meikle, W. P. S., 2008, A&A 483L, 47Google Scholar
Vink, J. S., 2009, astro-ph/0905.3338CrossRefGoogle Scholar
Vink, J. S. & de Koter, A., 2005, A&A 442, 587Google Scholar
Vink, J. S., de Koter, A., & Lamers, H. J. G. L. M., 2000, A&A 362, 295Google Scholar
Vink, J. S., Muijres, L. E., Anthonisse, B., et al. , 2011a, A&A 531, 132Google Scholar
Vink, J. S., Gräfener, G., & Harries, T. J., 2011b, A&A 536L, 10Google Scholar
Yoon, S.-C. & Langer, N., 2005, A&A 443, 643Google Scholar