Bow Shocks, Mach Disks and Entrainment in HH 46/47

Details Bow Shocks, Mach Disks and Entrainment in HH 46/47 Bow Shocks, Mach Disks and Entrainment in HH 46/47

Dec 1992

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1992aas...181.1704m&link_type=abstract

American Astronomical Society, 181st AAS Meeting, #17.04; Bulletin of the American Astronomical Society, Vol. 24, p.1147

Astronomy and Astrophysics

Astronomy

Scientific paper

The HH 46/47 system is among the brightest and best-studied of the optical bi-polar outflows emanating from newly formed stars. We have obtained detailed spectrophotometry of the blue-shifted lobe of HH 46/47 using the Rutgers/CTIO imaging Fabry-Perot on the CTIO 4-m telescope in the Hα and [S II]lambda lambda6716 ,6731 emission lines. Gaussian fits to ~ 10,000 line profiles map the kinematics of the HH 47 jet and working surfaces HH 47A and 47D. Monochromatic images of the [S II]lambda6716 /lambda6731 and [S II](lambda6716 + lambda6731 )/Hα line ratios survey the post-shock electron densities and excitation conditions throughout the entire flow volume. Both the outer working surface HH 47D and the inner working surface HH 47A show separate bow shock and Mach disk emission. We estimate shock velocities in each of these regions and find that HH 47A must move into a pre-shock medium that already has an outward velocity away from the stellar source of ~ 125 km s(-1) to explain the observed kinematics and excitation conditions. A simple ram pressure argument shows that the jet material is ~ 15 times denser than the ambient medium in HH 47D, but the jet material entering the inner working surface is only about half as dense as the pre-shock medium of HH 47A. Monochromatic images of the HH 46/47 jet show that at high radial velocities the jet appears clumpy but reasonably straight over large scales. However, the jet splits into two strands whose projected separation increases toward lower velocities. This behavior is the signature of a jet that goes fast down the middle and slower at the edges. It is not consistent with a jet that precesses either ballistically or due to magnetic confinement. The jet appears to be entraining the surrounding material, a conclusion also reached by Chernin & Masson (1991) to explain the bi-polar CO outflow. This may represent the first conclusive evidence for a common origin to the optical and CO outflows in a stellar jet.

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