Computer Science
Scientific paper
Jan 2001
adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2001iaus..205..274a&link_type=abstract
Galaxies and their Constituents at the Highest Angular Resolutions, Proceedings of IAU Symposium #205, held 15-18 August 2000 at
Computer Science
Scientific paper
The ``proplyds'' are bright, compact, emission-line knots surrounding low-mass stars in the Orion Nebula. An explanation for these objects is that the radiation from the main exciting source in the nebula, θ1 C Ori, is photoevaporating the circumstellar material around these low-mass stars. This photoevaporated flow then interacts with the stellar wind from θ1 C Ori. The interaction should produce a bowshock around the proplyd, and indeed, such bowshocks can be seen in HST images of the Orion Nebula. We present hydrodynamic simulations of the interaction between the transonic photoevaporating flow from an externally irradiated circumstellar disk and a stellar wind from a young, massive, hot star. Depending on where the global shock in the stellar wind is, this interaction will be with either a supersonic unshocked stellar wind, or a subsonic, hot shocked stellar wind. The results are compared with HST observations of the high-ionization emission arcs found in front of the proplyds in the Orion Nebula and can be used to deduce the position of the global shock in the stellar wind from the young massive star θ1 C Ori.
Arthur Jane S.
Garcia-Arredondo F.
Henney William J.
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