A 1000 AU Rotating Disk around the Massive Young Stellar Object G192.16-3.82

Details A 1000 AU Rotating Disk around the Massive Young Stellar Object G192.16-3.82 A 1000 AU Rotating Disk around the Massive Young Stellar Object G192.16-3.82

Oct 1999

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1999apj...523..690s&link_type=abstract

The Astrophysical Journal, Volume 523, Issue 2, pp. 690-700.

Astronomy and Astrophysics

Astronomy

52

Stars: Circumstellar Matter, Ism: H Ii Regions, Ism: Individual (G192.16-3.82), Ism: Jets And Outflows, Ism: Molecules, Stars: Formation

Scientific paper

We present evidence for a circumstellar disk around the luminous young stellar object G192.16-3.82. Observations of 2.6 mm, 7 mm, and 3.6 cm continuum emission and ^13CO, C^18O, and H_2O maser line emission support the interpretation that a 1000 AU rotating disk exists around the central B2 star. The disk major axis is roughly perpendicular to the outflow, and the maser velocities are consistent with Keplerian rotation. The mass of the disk plus circumstellar envelope traced by millimeter continuum emission is ~15 M_solar. The source is embedded in a 500 M_solar molecular cloud from which a massive outflow emerges. Updated outflow parameters yield a total flow mass of 95 M_solar and a mass flow rate of 5.6x10^-4 M_solar yr^-1. The outflow opening angle, defined by a ^13CO shell, is approximately 90 deg. A weak, one-sided, ionized jet emanates from the young stellar object system. The estimated momentum rate of the jet (~10^-3 M_solar km s^-1 yr^-1) is about a factor of 4 too low to power the flow. These results are consistent with the idea that the G192.16 outflow mechanism can be best characterized by a combination of a weak jet and a strong, wide-angle wind. Approximately 0.5" to the north of G192.16-3.82 is a band of 3.6 cm continuum emission and redshifted H_2O maser components which we interpret to be due to a newly discovered jet from the embedded object G192.16-3.82 N. The jet does not affect the dynamics of the massive outflow significantly which indicates that it is probably due to a low-mass young stellar object.

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