Smith, M.D. and Rosen, A. (2007) Hydrodynamic simulations of rotating molecular jets. Monthly Notices of the Royal Astronomical Society, 378 (2). pp. 691-700. ISSN 0035-8711.
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Molecular outflows and the jets which may drive them can be expected to display signatures associated with rotation if they are the channels through which angular momentum is extracted from material accreting on to protostars. Here, we determine some basic signatures of rapidly rotating flows through three-dimensional numerical simulations of hydrodynamic jets with molecular cooling and chemistry. We find that these rotating jets generate a broad advancing interface which is unstable and develops into a large swarm of small bow features. In comparison to precessing jets, there is no stagnation point along the axis. The greater the rotation rate, the greater the instability. On the other hand, velocity signatures are only significant close to the jet inlet since jet expansion rapidly reduces the rotation speed. We present predictions for atomic, H-2 and CO submillimetre images and spectroscopy including velocity channel maps and position-velocity diagrams. We also include simulated images corresponding to Spitzer IRAC band images and CO emission, relevant for APEX and eventual ALMA observations. We conclude that protostellar jets often show signs of slow precession but only a few sources display properties which could indicate jet rotation.
|Uncontrolled keywords:||hydrodynamics; shock waves; ISM : clouds; ISM : jets and outflows; ISM : molecules|
|Subjects:||Q Science > QB Astronomy
Q Science > QC Physics
|Divisions:||Faculties > Science Technology and Medical Studies > School of Physical Sciences > Centre for Astrophysics and Planetary Sciences
Faculties > Science Technology and Medical Studies > School of Physical Sciences
|Depositing User:||Suzanne Duffy|
|Date Deposited:||19 Mar 2008 08:38|
|Last Modified:||14 Jan 2010 14:06|
|Resource URI:||http://kar.kent.ac.uk/id/eprint/2311 (The current URI for this page, for reference purposes)|
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