Issue |
A&A
Volume 458, Number 1, October IV 2006
|
|
---|---|---|
Page(s) | 181 - 190 | |
Section | Interstellar and circumstellar matter | |
DOI | https://doi.org/10.1051/0004-6361:20053209 | |
Published online | 16 October 2006 |
Molecular outflows from G35.2-0.74N
1
School of Physics & Astronomy, University of Manchester, Sackville Street, PO Box 88, Manchester M60 1QD, UK e-mail: joseph@josephbirks.com; G.Fuller@manchester.ac.uk
2
Department of Astronomy, University of Maryland, College Park, MD 20742, USA
Received:
8
April
2005
Accepted:
6
July
2006
We present interferometric observations of the massive
star-forming region associated with G35.2-0.74N using the
Berkeley Illinois Maryland Association Array. With the aim of better
understanding the outflow in this region we observed
,
and the 2.7 mm continuum. The
and continuum emission peak close to the sources G35.2-0.74N
(G35.2N) and G35MM2 and indicate a mass of
~
of circumstellar material associated
with these sources. The 12CO traces a weak filament of
emission coincident with the radio and infrared jet from G35.2N but
the emission is dominated by an extended outflow with a NE-SW axis
which has a total mass of ~13
. Each lobe of this
extended outflow has a hollow shell structure and the location of
these shells makes the source G35MM2 a more likely candidate for the
source driving the outflow than G35.2N. The mass-velocity
distribution is calculated for several parts of the outflow. Fitting
these distributions with power laws some of the same break-points
are seen as previously identified in the
emission from the outflow. We conclude this
indicates the temperature dependence of emissivity is not
responsible for all the break-points seen and molecular dissociation
is a more plausible explanation for their origin. We model the
molecular outflow using the ZEUS-2D hydrodynamic code which we have
augmented so that it can also track the composition of the gas. We
find that a general hydromagnetic wind, without an enchanced, on
axis, jet-like component, can reproduce the shape of the observed
outflow. Models looking at the time evolution of the stellar wind
indicate that the structure of the outflow is dominated by the
initial wind conditions, rather than its later evolution. The models
also show that scaling the density of the wind profile effects the
apparent collimation of the resulting outflow. This may help explain
some of the apparent differences between outflows from high mass and
low mass young stars.
Key words: ISM: jets and outflows / ISM: individual objects: G35.2-0.7N / radio lines: ISM
© ESO, 2006
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