Abstract
We present high-resolution CO |$J=2\rightarrow1$| and HCO+|$J=3\rightarrow2$| maps of the Orion B molecular outflow source. The outflow appears to be unipolar, and shows evidence of acceleration of molecular gas at up to 0.6 pc from the driving star. The highest velocity material, as well as being furthest from the source, seems to lie close to the central axis of the flow, and it is likely that it is being accelerated by entrainment in an unobserved flow or jet emanating from the star. The HCO+ emission arises in the cloud core where the excitation temperature is about 25 K. Mass estimates are in accordance with a model in which the core has a kinetic temperature of 30–50 K, with no molecular depletion on to grains. This is in contrast to the recent suggestion that the core contains cold isothermal protostars.
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