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Interferometric identification of a pre-brownd dwarf

Abstract : It is not known whether brown dwarfs [stellar-like objects with masses less than the hydrogen-burning limit, 0.075 solar mass (M☉)] are formed in the same way as solar-type stars or by some other process. Here we report the clear-cut identification of a self-gravitating condensation of gas and dust with a mass in the brown-dwarf regime, made through millimeter interferometric observations. The level of thermal millimeter continuum emission detected from this object indicates a mass ~0.02 to 0.03 M☉, whereas the small radius, <460 astronomical units, and narrow spectral lines imply a dynamical mass of 0.015 to 0.02 M☉. The identification of such a pre-brown dwarf core supports models according to which brown dwarfs are formed in the same manner as hydrogen-burning stars
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Contributor : Bruno Savelli Connect in order to contact the contributor
Submitted on : Tuesday, September 17, 2013 - 12:08:00 PM
Last modification on : Wednesday, October 27, 2021 - 2:24:59 PM

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Philippe André, D. Ward-Thompson, Jane Greaves. Interferometric identification of a pre-brownd dwarf. Science & Engineering of Composite Materials, 2012, 337 (6090), pp.69-72. ⟨10.1126/science.1222602⟩. ⟨cea-00862686⟩



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