Aperture synthesis CS (J = 1-0) observations of the molecular outflow in NGC 2071 - Clumpy structure in a wind-driven shocked shell

Details Aperture synthesis CS (J = 1-0) observations of the molecular outflow in NGC 2071 - Clumpy structure in a wind-driven shocked shell Aperture synthesis CS (J = 1-0) observations of the molecular outflow in NGC 2071 - Clumpy structure in a wind-driven shocked shell

Aug 1992

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1992pasj...44..407k&link_type=abstract

PASJ: Publications of the Astronomical Society of Japan (ISSN 0004-6264), vol. 44, no. 4, p. 407-420.

Astronomy and Astrophysics

Astronomy

17

Interstellar Matter, Molecular Clouds, Molecular Flow, Nebulae, Carbon Monoxide, Emission Spectra, Hydrogen, Interstellar Gas, Red Shift

Scientific paper

We made aperture synthesis CS (J = 1-0) observations of an expanding clumpy shocked shell that was found around the redshifted CO outflow in NGC 2071 during our previous study (Kitamura et al., 1990). The size of the synthesized beam was about 11 x 10 arcsec. It has been revealed that the previously identified clumps in the shocked shell comprise several small subclumps. The sizes of the subclumps range from 0.01 to 0.05 pc, and the estimated mass from 1 to 10 solar masses. The central velocities of the subclumps are distributed over a velocity range of V(LSR) = 5 to 22 km/s; no distinct systematic structure has been seen in velocity space. The Rayleigh-Taylor instability seems to be the probable mechanism to form such subclumps in a shock-compressed shell, if the outflow is a decelerating energy-driven flow. Besides, several subclumps with a velocity width (i.e., a full width at zero intensity) of 4 to 8 km/s, which are resolved in velocity space, have been shown to be gravitationally unbound.

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