2005/01/07 by Neil H. Symington, Tim J. Harries, Ryuichi Kurosawa
Biochemistry, Genetics and Molecular Biology · Physics and Astronomy · #Astro and Planetary Science #Astrophysics and Star Formation Studies #Geomagnetism and Paleomagnetism Studies #astro-ph
paper · pdf · doi:10.1111/j.1365-2966.2004.08601.x
published as Mon.Not.Roy.Astron.Soc. 356 (2005) 1489 · 14 pages, 12 figures. Published in MNRAS
arxiv created 2005/01/07 · openalex publication_date 2005/01/13 · arxiv updated 2009/12/01 · openalex created_date 2025/10/10 · openalex updated_date 2026/07/28
We present hydrogen emission-line profile models of magnetospheric accretion on to 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 magnetohydrodynamic 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 the 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.