EPJ Web of Conferences
Volume 16, 2011Research, Science and Technology of Brown Dwarfs and Exoplanets: Proceedings of an International Conference held in Shangai on Occasion of a Total Eclipse of the Sun
|Number of page(s)||7|
|Section||Very Low-Mass Stars and Brown Dwarfs|
|Published online||18 July 2011|
SMA and CARMA observations of young brown dwarfs in ρ Ophiuchi and Taurus
1 Department of Physics, HCMIU, Vietnam National University Administrative Building, Block 6, Linh Trung Ward, Thu Duc District, HCM, Vietnam
2 Institute of Astronomy and Astrophysics, Academia Sinica, PO Box 23-141, Taipei 106, Taiwan
3 Harvard-Smithsonian Center for Astrophysics, Cambridge, MA 02138, USA
a e-mail: email@example.com
Molecular outflows provide vital information about the earliest stages in the birth of stars, studying the molecular outflow properties is therefore crucial for understanding how stars form. Brown dwarfs with masses between that of stars and planets are not massive enough to maintain stable hydrogen-burning fusion reactions during most of their lifetime. Their origins are subject to much debate in recent literature because their masses are far below the typical mass where core collapse is expected to occur. Based on Submillimeter Array (SMA) and Combined Array for Research in Millimeter-wave Astronomy (CARMA) observations, we present the first detections of bipolar molecular outflows from young brown dwarfs in ρ Ophiuchi and Taurus. Our results demonstrate that the bipolar molecular outflow operates down to brown dwarf masses, occurring in brown dwarfs as a scaled-down version of the universal process seen in young low-mass stars. This demonstrates that brown dwarfs and low-mass stars likely share the same formation mechanism.
© Owned by the authors, published by EDP Sciences, 2011
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