2001/12/04 by Y. Ulchin, O. Regev, Ulchin, Y. +4
Physics and Astronomy · #Astro and Planetary Science #Astrophysics and Star Formation Studies #astro-ph
paper · pdf · doi:10.48550/arxiv.astro-ph/0112085
21 pages, 4 figures; accepted for MNRAS (figure 4 is compressed and thus of slightly reduced quality)
arxiv created 2001/12/04 · arxiv updated 2009/12/01
The structure of accretion discs around magnetic T Tauri stars is numerically calculated using a particle hydrodynamical code, in which magnetic interaction is included in the framework of King's diamagnetic blob accretion model. Setting up the calculation so as to simulate the density structure of a quasi-steady disc in the equatorial plane of a T Tauri star, we find that the central star's magnetic field typically produces a central hole in the disc and spreads out the surface density distribution. We argue that this result suggests a promising mechanism for explaining the unusual flatness (IR excess) of T Tauri accretion disc spectra.