Emission-line profile modelling of structured T Tauri magnetospheres

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dc.creatorSymington, Neil H.
dc.creatorHarries, Tim J.
dc.creatorKurosawa, Ryuichi
dc.date2005-01-07
dc.date.accessioned2026-07-07T02:16:39Z
dc.date.available2026-07-07T02:16:39Z
dc.descriptionWe present hydrogen emission line profile models of magnetospheric accretion onto Classical T Tauri stars. The models are computed under the Sobolev approximation using the three-dimensional Monte Carlo radiative-transfer code TORUS. We have calculated four illustrative models in which the accretion flows are confined to azimuthal curtains - a geometry predicted by magneto-hydrodynamical simulations. Properties of the line profile variability of our models are discussed, with reference to dynamic spectra and cross-correlation images. We find that some gross characteristics of observed line profile variability are reproduced by our models, although in general the level of variability predicted is larger than that observed. We conclude that this excessive variability probably excludes dynamical simulations that predict accretion flows with low degrees of axisymmetry.
dc.description14 pages, 12 figures. Published in MNRAS
dc.identifierhttps://arxiv.org/abs/astro-ph/0501106
dc.identifierhttp://arxiv.org/abs/astro-ph/0501106
dc.identifierMon.Not.Roy.Astron.Soc. 356 (2005) 1489
dc.identifierdoi:10.1111/j.1365-2966.2004.08601.x
dc.identifier.urihttp://salesiana.dossiersoluciones.com/handle/123456789/8871
dc.subjectAstrophysics
dc.titleEmission-line profile modelling of structured T Tauri magnetospheres
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