2006/03/09 by P. D. Klaassen, Pamela Klaassen, R. Plume +6 · 2 citations
Physics and Astronomy · #Astrophysical Phenomena and Observations #Astrophysics and Star Formation Studies #Stellar, planetary, and galactic studies #astro-ph
paper · pdf · doi:10.1086/504146
published as Astrophys.J.648:1079-1089,2006 · 27 Pages, 9 Figures, Accepted to ApJ. For full (High) resolution figures, please see http://www.ism.ucalgary.ca/~pamela/papers/index.html
arxiv created 2006/03/09 · openalex publication_date 2006/09/08 · arxiv updated 2009/12/01 · openalex created_date 2016/06/24 · openalex updated_date 2026/08/01
We have obtained maps of the large-scale outflow associated with the UC H II region G5.89-0.39 in CO and 13 CO ( J = 3-2), SiO ( J = 8-7, J = 5-4), SO 2 ( J = 13 2,12 -13 1,13 ), 13 and H 13 CO + ( J = 4-3). From these maps we have been able to determine the mass (3.3 M ☉ ), momentum (96 M ☉ km s -1 ), energy (3.5 × 10 46 ergs), mechanical luminosity (141 L ☉ ), and mass-loss rate (~ 1 × 10 -3 M ☉ yr -1 ) in the large-scale outflow. The observationally derived parameters were used to guide three-dimensional magnetohydrodynamic models of the jet-entrained outflow. Through the combination of observations and simulations, we suggest that the large-scale outflow may be inclined by approximately 45° to the line of sight, and that the jet entraining the observed molecular outflow may have been active for as little as 1000 years, half the kinematic age of the outflow.