Evidence for Pressure Driven Flows and Turbulent Dissipation in the Serpens NW Protocluster

Details Evidence for Pressure Driven Flows and Turbulent Dissipation in the Serpens NW Protocluster Evidence for Pressure Driven Flows and Turbulent Dissipation in the Serpens NW Protocluster

2000-02-14

arxiv.org/abs/astro-ph/0002288v1

Astronomy and Astrophysics

Astrophysics

Accepted for publication in the Astrophysical Journal 26 pages, 10 figures

Scientific paper

10.1086/309084

We have mapped the dense gas distribution and dynamics in the NW region of the Serpens molecular cloud in the CS(2-1) and N2H+(1-0) lines and 3 mm continuum using the FCRAO telescope and BIMA interferometer. 7 continuum sources are found. The N2H+ spectra are optically thin and fits to the 7 hyperfine components are used to determine the distribution of velocity dispersion. 8 cores, 2 with continuum sources, 6 without, lie at a local linewidth minimum and optical depth maximum. The CS spectra are optically thick and generally self-absorbed over the full 0.2 pc extent of the map. We use the line wings to trace outflows around at least 3, and possibly 4, of the continuum sources, and the asymmetry in the self-absorption as a diagnostic of relative motions between core centers and envelopes. The quiescent regions with low N2H+ linewidth tend to have more asymmetric CS spectra than the spectra around the continuum sources indicating higher infall speeds. These regions have typical sizes ~5000 AU, linewidths ~0.5 km/s, and infall speeds ~0.05 km/s. The correlation of CS asymmetry with N2H+ velocity dispersion suggests that the inward flows of material that build up pre-protostellar cores are driven at least partly by a pressure gradient rather than by gravity alone. We discuss a scenario for core formation and eventual star forming collapse through the dissipation of turbulence.

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