Journal Article

MHD modelling of a disc wind from a high-mass protobinary: the case of Orion Source I

B. Vaidya and C. Goddi

in Monthly Notices of the Royal Astronomical Society: Letters

Published on behalf of The Royal Astronomical Society

Volume 429, issue 1, pages L50-L54
Published in print February 2013 |
Published online November 2012 | e-ISSN: 1745-3933 | DOI:

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Very Long Baseline Interferometry (VLBI) observations of SiO masers in Orion Source I has enabled for the first time to resolve the outflow from a high-mass protostar in the launch and collimation region. Therefore, Source I provides a unique laboratory to study mass loss and mass accretion in a high-mass protostar. We numerically simulate the dynamics of the disc wind inside 100 au from Source I. This enables us to investigate the balance of different forces (gravitational, magnetic, thermal) regulating gas dynamics in massive star formation. In this work, we adopt magnetohydrodynamic (MHD) disc-wind models to explain the observed properties of the disc wind from Orion Source I. The central source is assumed to be a binary composed of two 10 M stars in a circular orbit with an orbital separation of 7 au. High-resolution ideal MHD wind-launching simulations (which prescribe disc as a boundary) are performed using the pluto code. The simulations are allowed to run until a steady state is obtained. MHD-driven disc wind provides a consistent model for the wide-angle flow from Source I probed by SiO masers, reproducing the bipolar morphology, the velocity amplitude and rotational profile, the physical conditions, and the magnetic field strength.

Keywords: MHD; methods: numerical; ISM: jets and outflows

Journal Article.  3455 words.  Illustrated.

Subjects: Astronomy and Astrophysics

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