Impact of Stellar Mass Loss on the Jet of Centaurus A

Details Impact of Stellar Mass Loss on the Jet of Centaurus A Impact of Stellar Mass Loss on the Jet of Centaurus A

Feb 2010

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2010head...11.0506n&link_type=abstract

American Astronomical Society, HEAD meeting #11, #5.06; Bulletin of the American Astronomical Society, Vol. 41, p.657

Astronomy and Astrophysics

Astronomy

Scientific paper

The radio jet of Centaurus A is well resolved in deep Chandra X-ray images, which provide tight constraints on its width and bounding pressure profiles. These quantities overdetermine a simple flow model for the jet, showing that Bernoulli's theorem fails. This implies significant dissipation within the jet, the likely cause of which is mass entrainment. The required rate of entrainment is remarkably close to the rate of stellar mass loss within the body of the jet. The number of X-ray knots within the jet is also similar to the number of AGB stars expected to dominate the stellar mass loss. If mass entrainment is dominated by stellar mass loss, jet width is sensitive to initial and boundary conditions, so that small changes in the environment can transform the jet into a lobe, which may account for the asymmetric radio morphology of Centaurus A.

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