Effects of Shear and Magnetic Fields on Molecular Cloud Formation in the Flow-Driven Picture in 2D

Details Effects of Shear and Magnetic Fields on Molecular Cloud Formation in the Flow-Driven Picture in 2D Effects of Shear and Magnetic Fields on Molecular Cloud Formation in the Flow-Driven Picture in 2D

Jan 2012

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2012aas...21934902h&link_type=abstract

American Astronomical Society, AAS Meeting #219, #349.02

Astronomy and Astrophysics

Astronomy

Scientific paper

We present a parameter study addressing the ramifications of shear in the flow-driven scenario of molecular cloud formation. Previous studies in two and three dimensions of this cloud and core formation picture have not included the exploration of a more realistic scenario of flows colliding at an angle. The introduction of shear is accomplished by varying the angle of the initial interface between two supersonic colliding flows, which introduces additional overall angular momentum to the molecular cloud. Shear in these flows can also inhibit global and local collapse, but still permits the formation of dense cores at regularly spaced intervals in the final cloud. In this work we are primarily concerned with the effects on the energy balance and angular momentum distribution of the resulting protostellar cores, and how these outcomes change as magnetic fields are included. A secondary concern is how the overall core formation rate is affected by the changes in angle and initial Mach number of the flow. These simulations are done in AstroBEAR, an MHD code capable of adaptive mesh refinement with self-gravity.

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