Hostname: page-component-848d4c4894-m9kch Total loading time: 0 Render date: 2024-05-10T15:09:52.026Z Has data issue: false hasContentIssue false
  • English
  • Français

Between Cool Stars and Hot Planets: Origins of Brown Dwarfs

Published online by Cambridge University Press:  26 May 2016

Ray Jayawardhana
Ray Jayawardhana*
Affiliation:
Department of Astronomy, University of Michigan, 830 Dennison Building, Ann Arbor, MI 48109, U.S.A.

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.

Brown dwarfs, which straddle the mass range between stars and planets, appear to be common both in the solar neighborhood and in star-forming regions. Their ubiquity makes the question of their origin an important one both for our understanding of brown dwarfs themselves as well as for theories on the formation of stars and planets. Studies of young sub-stellar objects could provide valuable insight into their formation and early evolution. Here I report on the latest results from our observational programs at Keck, VLT and Magellan on the disk and accretion properties of young brown dwarfs. We find compelling evidence that they undergo a T Tauri phase analogous to that of their stellar counterparts.

Type
Part 6: Low Mass Stellar Magnetic Activity and Evolution
Information
Symposium - International Astronomical Union , Volume 219: Stars as Suns : Activity, Evolution and Planets , 2004 , pp. 296 - 300
Copyright
Copyright © Astronomical Society of the Pacific 2004 

References

Barrado y Navascués, D., Mohanty, S., & Jayawardhana, R. 2003, ApJ, submitted.Google Scholar
Bate, M. R., Bonnell, I. A. & Bromm, V. 2002, MNRAS, 336, 705.CrossRefGoogle Scholar
Bessell, M. S. & Brett, J. M. 1988, PASP, 100, 1134.Google Scholar
Fernández, M. & Comerón, F. 2001, A&A 380, 264.Google Scholar
Haisch, K. E. Jr., Lada, E. A. & Lada, C. J. 2001, AJ, 121, 2065.Google Scholar
Jayawardhana, R., Mohanty, S., & Basri, G. 2002, ApJ, 578, L141.CrossRefGoogle Scholar
Jayawardhana, R., Mohanty, S., & Basri, G. 2003, ApJ, 592, 282.CrossRefGoogle Scholar
Jayawardhana, R., Ardila, D.R., Stelzer, B. & Haisch, K.E. Jr. 2003, AJ, 126, 1515.Google Scholar
Leggett, S. K., et al. 2002, ApJ, 564, 452.Google Scholar
Liu, M. C., Najita, J. & Tokunaga, A. T. 2003, ApJ, 585, 372.Google Scholar
Mohanty, S., Jayawardhana, R., & Barrado y Navascués, D. 2003, ApJ, 593, L109.Google Scholar
Muench, A.A., et al. 2001, ApJ, 558, L51.CrossRefGoogle Scholar
Natta, A., et al. 2002, A&A, 393, 597.Google Scholar
Neuhäuser, R., et al. 2002, A&A, 384, 999.Google Scholar
Padoan, P. & Nordlund, A. 2003, ApJ, submitted.Google Scholar
Reipurth, B. & Clarke, C. 2001, AJ, 122, 432.CrossRefGoogle Scholar