2020/06/23 by Florian Ragossnig, Ernst A. Dorfi, E. A. Dorfi +8 · 8 citations
Mathematics · Physics and Astronomy · #Algorithm #Computation #Computational science #Computer science #Mathematics #Nuclear physics research studies #Parallel computing #Quantum chaos and dynamical systems #astro-ph.EP #physics.comp-ph
paper · pdf · doi:10.1016/j.cpc.2020.107437
published in Computer Physics Communications 256, 107437 (Elsevier BV) · for details check https://authors.elsevier.com/tracking/article/details.do?aid=107437&jid=COMPHY&surname=Ragossnig
arxiv created 2020/06/23 · openalex publication_date 2020/06/26 · arxiv updated 2020/08/26 · openalex created_date 2025/10/10 · openalex updated_date 2026/08/05
We present an implicit numerical method to solve the time-dependent equations of radiation hydrodynamics (RHD) in axial symmetry assuming hydrostatic equilibrium perpendicular to the equatorial plane (1+1D) of a gaseous disk. The equations are formulated in conservative form on an adaptive grid and the corresponding fluxes are calculated by a spacial second order advection scheme. Self-gravity of the disk is included by solving the Possion equation. We test the resulting numerical method through comparison with a simplified analytical solution as well as through the long term viscous evolution of protoplanetary disk when due to viscosity matter is transported towards the central host star and the disk depletes. The importance of the inner boundary conditions on the structural behaviour of disks is demonstrated with several examples.