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Two-Wind Interaction Models of the Proplyds in the Orion Nebula

Published online by Cambridge University Press:  25 May 2016

W. J. Henney  and
S. J. Arthur
W. J. Henney
Affiliation:
Instituto de Astronomía, UNAM, Unidad Morelia, J. J. Tablada 1006, 58090 Morelia, Michoacán, México
S. J. Arthur
Affiliation:
Instituto de Astronomía, UNAM, Unidad Morelia, J. J. Tablada 1006, 58090 Morelia, Michoacán, México

Abstract

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Many low-mass stars in the Orion nebula are associated with very compact (≃ 1 arcsec) emission knots, known variously as proplyds, PIGs or LV knots. Some of these knots are teardrop-shaped, with “tails” pointing away from the massive star θ1 Ori C, which is the principal exciting star of the nebula. We discuss models of such knots, which invoke the interaction of the fast stellar wind from θ1 Ori C with a transonic photoevaporated flow from the surface of an accretion disk around a young low-mass star. We review previous analytic work and compare the results of the model with the observed brightnesses, morphologies and emission line profiles of the knots, as well as presenting new results from numerical hydrodynamical simulations.

Type
V. Low- and High-Mass Protostars and Their Environment
Information
Symposium - International Astronomical Union , Volume 182: Herbig-Haro Flows and the Birth of Low Mass Stars , 1997 , pp. 561 - 570
Copyright
Copyright © Kluwer 1997 

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