Simulations of Accretion onto Magnetized Stars: Results of 3D MHD Simulations and 3D Radiative Transfer

2014/01/20 by M. M. Romanova, Marina Romanova, Romanova, Marina +2
Physics and Astronomy · #Astro and Planetary Science #Astrophysics and Star Formation Studies #FOS: Physical sciences #Solar and Stellar Astrophysics (astro-ph.SR) #Stellar, planetary, and galactic studies #astro-ph.SR

paper · pdf · doi:10.48550/arxiv.1401.4761

6 pages, 5 figures, to appear in the proceedings of ASTRONUM-2013 meeting: "8th International Conference on Numerical Modeling of Space Plasma Flows", Biarritz, France, July 1-5, 2013

arxiv created 2014/01/20 · openalex publication_date 2014/01/20 · arxiv updated 2014/01/21 · openalex created_date 2016/06/24 · openalex updated_date 2026/07/28

Abstract

We discuss the results of modelling of young magnetized stars, where matter flow is calculated using the three-dimensional (3D) magneto-hydrodynamic (MHD) "Cubed Sphere" code, and the spectra are calculated using the 3D Monte Carlo radiative transfer code "TORUS". Two examples of modelling are shown: (1) accretion onto stars in stable and unstable regimes, and (2) accretion to a young star V2129 Oph, modelled with realistic parameters.

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