Structure and physical properties of the bipolar outflow in L1551

Details Structure and physical properties of the bipolar outflow in L1551 Structure and physical properties of the bipolar outflow in L1551

Aug 1985

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1985apj...295..490s&link_type=abstract

Astrophysical Journal, Part 1 (ISSN 0004-637X), vol. 295, Aug. 15, 1985, p. 490-500.

Astronomy and Astrophysics

Astronomy

97

Astronomical Maps, Carbon Monoxide, Gas Dynamics, Nebulae, Stellar Mass Ejection, Emission Spectra, Molecular Clouds, Molecular Gases, Red Shift, Stellar Winds

Scientific paper

The high-velocity C-12O J = 1-0 emission in L1551 on a 1-arcmin grid has been mapped, using the 14 m telescope of the Five College Radio Astronomy Observatory. Also obtained are data during a lunar occultation of this outflow which permits a resolution of 7 arcsec along the moon's path. Finally, observations of C-13O and CS have been made to trace regions of larger column density and density both within the high-velocity outflow and in the ambient cloud. Analysis of the entire data set suggests that the bulk of the high-velocity CO emission arises from a thin shell of gas surrounding a cavity in the molecular cloud that is presently filled by the stellar wind from IRS 5. This shell of gas has been accelerated by the stellar wind and is moving radially away from IRS 5 at 12 km/s. In addition, the shell appears to be expanding at about 4 km/s, possibly due to the pressure exerted by the hot stellar wind. The combination of these motions gives rise to the complex kinematic structure of the high-velocity gas near IRS 5.

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