Naomi Hirano et al 2004 ApJ 616 L43 doi:10.1086/424382
Naomi Hirano1, Hiroko Shinnaga2, Dinh-V-Trung1, David Fong2, Eric Keto3, Nimesh Patel3, Chunhua Qi3, Ken Young3, Qizhou Zhang3 and Junhui Zhao3
Show affiliationsUsing the partially completed Submillimeter Array with five antennas, we have observed the CO J = 2-1 and 3-2 emission from the envelope surrounding the carbon star V Hya. The high angular resolution (2''-4'') maps show that V Hya is powering a bipolar molecular jet with an extreme velocity of 70-185 km s-1. The axis of this high-velocity jet is perpendicular to the major axis of the flattened disklike envelope, which is expanding with a velocity of ~16 km s-1. There is a third kinematic component, a medium-velocity wind with a deprojected velocity of 40-120 km s-1 moving along the disk plane. Both the high-velocity jet and the medium-velocity wind have a dynamical timescale of a few hundred years. The flattened structure and the collimated jet observed in V Hya suggest that the formation of asymmetrical structure proceeds while the central star is still in the asymptotic giant branch phase.
ISM: individual (V Hydrae); ISM: jets and outflows; ISM: molecules; stars: AGB and post-AGB
Issue 1 (2004 November 20)
Received 2004 May 1, accepted for publication 2004 July 14
Published 2004 October 28
Naomi Hirano et al 2004 ApJ 616 L43
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