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Radiative-transfer modelling of funnel flows

Published online by Cambridge University Press:  01 May 2007

Tim J. Harries
Tim J. Harries*
Affiliation:
School of Physics, University of Exeter, Stocker Road, Exeter, EX4 4QL, UK email: th@astro.ex.ac.uk
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Abstract

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Emission line profiles from pre-main-sequence objects accreting via magnetically-controlled funnel flows encode information on the geometry and kinematics of the material on stellar radius scales. In order to extract this information it is necessary to perform radiative-transfer modelling of the gas to produce synthetic line profiles. In this review I discuss the physics that needs to be included in such models, and the numerical methods and assumptions that are used to render the problem tractable. I review the progress made in the field over the last decade, and summarize the main successes and failures of the modelling work.

Keywords

Radiative transferline: formationstars: formationstars: magnetic fields
Type
Contributed Papers
Information
Proceedings of the International Astronomical Union , Volume 3 , Symposium S243: Star-Disk Interaction in Young Stars , May 2007 , pp. 83 - 94
Copyright
Copyright © International Astronomical Union 2007

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