Astronomy and Astrophysics – Astronomy
Scientific paper
Jul 1994
adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1994mnras.269..447d&link_type=abstract
Monthly Notices of the Royal Astronomical Society, Vol. 269, NO. 2/JUL15, P. 447, 1994
Astronomy and Astrophysics
Astronomy
9
Scientific paper
It has been proposed that the cometary head-tail system of the red supergiant IRS7 near the Galactic Centre is produced by the interaction of a hypersonic galactocentric wind with the stellar envelope. If, however, the envelope is impermeable to the wind and mass is ablated from its boundary surface, such an interaction produces a `stubby' tail, and the observed long one cannot be dynamically related to the cometary head. We propose that the wind interacts with a clumpy permeable envelope and is decelerated primarily in bowshocks around clumps. Thus the ram pressure of the Galactic Centre wind plays no role in determining the head size. The mass-loaded wind cools efficiently by radiation, and the flow is momentum- rather than energy-driven. As a result, the tail does not expand much sideways, and has lateral dimensions determined effectively by the scalesize of the mass-loading region, which in turn marks the cometary head. Key words: hydrodynamics - shock waves - circumstellar matter - stars: individual: IRS7 - ISM: jets and outflows - Galaxy: centre.
Dyson John E.
Hartquist Thomas W.
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