Herschel/SPIRE observations of the TWA brown dwarf disc 2MASSW J1207334−393254†

  1. B. Riaz1,*,
  2. G. Lodato2,
  3. D. Stamatellos3,
  4. J. E. Gizis4

Article first published online: 21 FEB 2012

DOI: 10.1111/j.1745-3933.2012.01225.x

Issue

Monthly Notices of the Royal Astronomical Society: Letters

Monthly Notices of the Royal Astronomical Society: Letters

Volume 422, Issue 1, pages L6–L10, May 2012

Additional Information

How to Cite

Riaz, B., Lodato, G., Stamatellos, D. and Gizis, J. E. (2012), Herschel/SPIRE observations of the TWA brown dwarf disc 2MASSW J1207334−393254. Monthly Notices of the Royal Astronomical Society: Letters, 422: L6–L10. doi: 10.1111/j.1745-3933.2012.01225.x

Author Information

  1. 1

    Centre for Astrophysics Research, Science & Technology Research Institute, University of Hertfordshire, Hatfield AL10 9AB

  2. 2

    Dipartimento di Fisica, Università Degli Studi di Milano, Via Celoria, 16, Milano 20133, Italy

  3. 3

    School of Physics & Astronomy, Cardiff University, Cardiff CF24 3AA

  4. 4

    Department of Physics and Astronomy, University of Delaware, Newark, DE 19716, USA

*Herschel is an ESA space observatory with science instruments provided by European-led Principal Investigator consortia and with important participation from NASA.
E-mail: b.riaz@herts.ac.uk

Publication History

  1. Issue published online: 19 APR 2012
  2. Article first published online: 21 FEB 2012
  3. Accepted 2012 January 18. Received 2012 January 17; in original form 2011 December 24

SEARCH

SEARCH BY CITATION

ARTICLE TOOLS

View Full Article (HTML) Get PDF (307K)

Keywords:

  • brown dwarfs;
  • circumstellar matter;
  • stars: individual: 2MASSW J1207334−393254;
  • stars: low-mass

ABSTRACT

We present Herschel/SPIRE observations for the 2MASS 1207334−393254 (2M1207) system. Based on radiative transfer modelling of near-infrared to submillimetre data, we estimate a disc mass of 3 ± 2 MJup and an outer disc radius of 50–100 au for the 2M1207A disc. The relative disc mass for 2M1207A is similar to the T Tauri star TW Hya, which indicates that massive discs are not underabundant around substellar objects. In probing the various formation mechanisms for this system, we find that core accretion is highly uncertain mainly due to the large separation between the primary and the companion. Disc fragmentation could be a likely scenario based on analytical models, and if the disc initially was more massive than its current estimate. Considering that the TW Hydrae Association (TWA) is sparsely populated, this system could have formed via one of the known binary formation mechanisms (e.g. turbulent fragmentation of a core) and survived disruption at an early stage.

View Full Article (HTML) Get PDF (307K)