Hostname: page-component-586b7cd67f-gb8f7 Total loading time: 0 Render date: 2024-11-20T10:42:22.619Z Has data issue: false hasContentIssue false
  • English
  • Français

The formation of brown dwarfs

Published online by Cambridge University Press:  18 January 2010

Ant Whitworth ,
Dimitri Stamatellos ,
Steffi Walch ,
Murat Kaplan ,
Simon Goodwin ,
David Hubber  and
Richard Parker
Ant Whitworth
Affiliation:
School of Physics & Astronomy, Cardiff University, Cardiff CF24 3AA, UK email: [email protected]
Dimitri Stamatellos
Affiliation:
School of Physics & Astronomy, Cardiff University, Cardiff CF24 3AA, UK email: [email protected]
Steffi Walch
Affiliation:
School of Physics & Astronomy, Cardiff University, Cardiff CF24 3AA, UK email: [email protected]
Murat Kaplan
Affiliation:
School of Physics & Astronomy, Cardiff University, Cardiff CF24 3AA, UK email: [email protected]
Simon Goodwin
Affiliation:
Department of Physics & Astronomy, University of Sheffield, Sheffield S3 7RH, UK
David Hubber
Affiliation:
Department of Physics & Astronomy, University of Sheffield, Sheffield S3 7RH, UK
Richard Parker
Affiliation:
Department of Physics & Astronomy, University of Sheffield, Sheffield S3 7RH, UK
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.

We argue that brown dwarfs (BDs) and planemos form by the same mechanisms as low-mass hydrogen-burning stars, but that as one moves to lower and lower masses, an increasing fraction of these objects is formed by fragmentation of the outer parts (R ≳ 100 AU) of protostellar accretion discs around more massive primary protostars, which in turn formed in their own very-low-mass prestellar cores. Numerical simulations of disc fragmentation with realistic thermodynamics show that low-mass objects are readily formed by fragmentation of short-lived massive, extended protostellar accretion discs. Such objects tend subsequently to be liberated into the field at low speed, due to mutual interactions with the primary protostar. Many (~20%) are in low-mass (M1 + M2 < 0.2M⊙) binary systems with semi-major axes a ~ 1 to 2 AU or ~200 AU and mass ratios q ≡ M2/M1 ≳ 0.7. Most of the brown dwarfs have sufficiently large attendant discs to sustain accretion and outflows. Most of the BDs that remain bound to the primary protostar have wide orbits (i.e., there is a BD desert), and these BDs also have a significantly higher probability of being in a BD/BD binary system than do the brown dwarfs that are liberated into the field (just as observed). In this picture, the multiplicity statistics and velocity dispersion of brown dwarfs are largely determined by the eigen evolution of a small-N system, born from a single prestellar core, rather than the larger-scale dynamics of the parent cluster. Consequently, many of the statistical properties of brown dwarfs should not differ very much from one star-formation region to another.

Keywords

accretionaccretion disksgravitationhydrodynamicsradiative transferstellar dynamicsbinaries: generalstars: formationstars: low-massbrown dwarfs
Type
Contributed Papers
Information
Proceedings of the International Astronomical Union , Volume 5 , Symposium S266: Star clusters: basic galactic building blocks throughout time and space , August 2009 , pp. 264 - 271
Copyright
Copyright © International Astronomical Union 2010

References

André, P., Belloche, A., Motte, F., & Peretto, N. 2007, A&A, 472, 519Google Scholar
Bate, M. R., Bonnell, I. A., & Bromm, V. 2003, MNRAS, 339, 577Google Scholar
Burgasser, A. J., Kirkpatrick, J. D., & Lowrance, P. J. 2005, AJ, 129, 2849Google Scholar
Burgasser, A. J., Reid, I. N., Siegler, N., Close, L., Allen, P., Lowrance, P. J., & Gizis, J. 2007, in: Reipurth, B., Jewitt, D. & Keil, K. (eds.), Protostars & Planets V, p. 427, Tucson: University of Arizona PressGoogle Scholar
Chabrier, G. 2003, PASP, 115, 763Google Scholar
Gammie, C. A. 2001, ApJ, 553, 174CrossRefGoogle Scholar
Goldreich, P. & Lynden–Bell, D. 1965, MNRAS, 130, 97Google Scholar
Goodwin, S. P., Whitworth, A. P., & Ward–Thompson, D. 2004, A&A, 414, 633Google Scholar
Hennebelle, P. & Chabrier, G. 2008, ApJ, 684, 395CrossRefGoogle Scholar
Hester, J. J., et al. 1996, AJ, 111, 2349CrossRefGoogle Scholar
Klessen, R. & Burkert, A. 2002, ApJS, 128, 287Google Scholar
Kroupa, P. 2002, Science, 295, 82CrossRefGoogle Scholar
Luhman, K., Joergens, V., Lada, C., Muzerolle, J., Pascucci, I., & White, R. 2007, in: Reipurth, B., Jewitt, D. & Keil, K. (eds.), Protostars & Planets V, p. 443, Tucson: University of Arizona PressGoogle Scholar
Padoan, P. & Nordlund, Å 2002, ApJ, 576, 870Google Scholar
Reipurth, B. & Clarke, C. J. 2001, AJ, 122, 432Google Scholar
Stamatellos, D., Whitworth, A. P., Bisbas, T., & Goodwin, S. P. 2007, A&A, 475, 37Google Scholar
Stamatellos, D., Hubber, D. A., & Whitworth, A. P. 2007, MNRAS (Letters), 382, L30Google Scholar
Stamatellos, D. & Whitworth, A. P. 2009a, MNRAS, 392, 413Google Scholar
Stamatellos, D. & Whitworth, A. P. 2009b, MNRAS, in press (arXiv:0908.2247)Google Scholar
Toomre, A. 1964, ApJ, 139, 1217CrossRefGoogle Scholar
Whitworth, A. P., Bate, M. R., Nordlund, Å., Reipurth, B., & Zinnecker, H. 2007, in: Reipurth, B., Jewitt, D. & Keil, K. (eds.), Protostars & Planets V, p. 459, Tucson: University of Arizona PressGoogle Scholar
Whitworth, A. P. & Stamatellos, D. 2006, A&A, 458, 817Google Scholar
Whitworth, A. P. & Zinnecker, H. 2004, A&A, 427, 299Google Scholar