The Disk and Outflow in G192.16: Are Massive Outflows and Accretion Disks Different from those in Low-Mass YSOs?

Details The Disk and Outflow in G192.16: Are Massive Outflows and Accretion Disks Different from those in Low-Mass YSOs? The Disk and Outflow in G192.16: Are Massive Outflows and Accretion Disks Different from those in Low-Mass YSOs?

Dec 1998

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1998aas...193.7301s&link_type=abstract

American Astronomical Society, 193rd AAS Meeting, #73.01; Bulletin of the American Astronomical Society, Vol. 30, p.1361

Astronomy and Astrophysics

Astronomy

Scientific paper

We present the discovery of a circumstellar disk around the luminous Young Stellar Object (YSO) G192.16-3.82. Observations of 2.6 mm, 7 mm, and 3.6 cm continuum emission and (13) CO, C(18) O, and H_2O maser line emission using the Owens Valley Radio Observatory and the Very Large Array reveal a 1000 AU, rotating disk around the central B2 star. The mass of the disk plus envelope is ~ 20 Msun. The YSO is embedded in a 500 Msun molecular cloud from which a massive outflow emerges. Updated outflow parameters yield a total flow mass of 95 Msun and a mass flow rate of 5.6 x 10(-4) Msun yr(-1) . The outflow opening angle, defined by a (13) CO shell centered on the YSO, is ~ 90(deg) . There is no evidence for the presence of a collimated jet, thus, the massive outflow is most likely produced by a powerful, moderately collimated wind with sufficient momentum to create a flow that is greater than 10 pc from end-to-end with ~ 10 times the mass of the central star. Approximately 0farcs5 to the north of the massive G192.16 YSO and disk is a stripe of 3.6 cm continuum emission along with red-shifted H_2O maser components which we interpret to be due to a jet emanating from a newly discovered YSO, G192.16 N. This jet/outflow system does not appear to significanty affect the dynamics of the massive outflow, hence, it is probably due to a low-mass YSO.

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