Compact Outflows Associated with TMC-1 and TMC-1A

Details Compact Outflows Associated with TMC-1 and TMC-1A Compact Outflows Associated with TMC-1 and TMC-1A

Nov 1996

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1996apj...471..308c&link_type=abstract

Astrophysical Journal v.471, p.308

Astronomy and Astrophysics

Astronomy

44

Ism: Jets And Outflows, Ism: Individual Alphanumeric: Tmc-1, Ism: Individual Alphanumeric: Tmc-1A, Infrared: Ism: Continuum, Ism: Reflection Nebulae, Stars: Formation

Scientific paper

High spatial resolution observations are presented of the compact outflows associated with the young protostars TMC-1 (IRAS 04381+2540) and TMC-1A (IRAS 04365+2535) in Taurus. Emission in CO(1-0) imaged with the Owens Valley Millimeter Array shows the outflow lobes to be conical close to the star. Analysis of the outflow dynamics indicates that these objects are low-luminosity versions of the energetic outflows more commonly observed. Near-infrared images at H and K bands show a close correspondence between reflection nebulosity and the location of high-velocity gas and suggest the outflow cavity is evacuated, as do position-velocity diagrams of the CO(2-1). Comparison of the j = 1-0 transition with emission in the 2-1 line indicates that the excitation temperature in the high-velocity gas is higher than the surrounding Taurus cloud. We place limits on the inclination of both objects by comparing the data with theoretical outflow models and conclude that i ˜ 40°-70°for both objects. The deprojected opening angles of the outflow cones are then in the range 30°-40°.
None of the current outflow models satisfactorily explains the results for TMC-1 and TMC-1A, which are among the youngest class I sources in Taurus. We find their outflow structure shares many similarities with the more obscured and possibly younger class 0 objects, B335 and L1448-C. The main difference is the lower mechanical luminosities of the TMC-1 and TMC-1A outflows, reflecting a factor of 3-4 smaller linear extent and velocity and a factor of 10-20 lower mass than the L1448-C molecular jet source. Taken together, the four protostars share the common properties of (1) conical outflow lobes close to the star, (2) evacuated outflow cavities, and (3) relatively wide 30°-40° opening angles. A successful theory of young stellar outflows must be able to explain these characteristics.

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