Mathematics – Logic
Scientific paper
Jan 2011
adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2011aas...21713104t&link_type=abstract
American Astronomical Society, AAS Meeting #217, #131.04; Bulletin of the American Astronomical Society, Vol. 43, 2011
Mathematics
Logic
Scientific paper
The morphology and kinematics of infalling envelopes around protostars determine the structure of the forming protostellar disk and reflect back on the initial properties of their parent dark clouds. Axisymmetric envelopes are often used in comparison to observations due to simplicity; however, 8 micron shadow images from Spitzer show that the dense envelopes around Class 0 protostars are generally morphologically complex, often filamentary, and frequently non-axisymmetric. The observed envelope structure indicates a likely origin in turbulent cloud structure rather than a quasi-static formation and increase the likelihood of fragmentation during collapse, forming close binaries. This complex complex envelope structure is observed in regions spatially distinct from outflow cavities, and often show no systematic alignment perpendicular to the cavities. To further characterize these systems, I have observed them in the dense gas tracers N2H+, N2D+, and ammonia which closely follow the extinction morphology. The magnitude of the velocity gradients on R 10000 AU scales indicates that the velocity structure, which has historically interpreted as rotation, may really be large-scale infall. Furthermore, several systems show large velocity gradients and/or linewidths near the protostar, as expected for infall or increased rotational velocity in the inner envelope. Comparisons with three-dimensional filamentary and symmetric rotating collapse models indicate that the position-velocity structure seen in many systems is better reproduced by filaments than sheets or spheres. These results strongly show that the structure of the envelope must be considered when interpreting the velocity field.
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