Three-temperature radiation hydrodynamics with PLUTO: Tests and applications to protoplanetary disks

Abstract

In circumstellar disks around T Tauri stars, visible and near-infrared stellar irradiation is intercepted by dust at the disk's optical surface and reprocessed into thermal infrared; this subsequently undergoes radiative diffusion through the optically thick bulk of the disk. The gas component -- overwhelmingly dominant by mass, but contributing little to the opacity -- is heated primarily by gas-grain collisions. In hydrodynamical simulations, however, typical models for this heating process (local isothermality, $\beta$-cooling, two-temperature radiation hydrodynamics) incorporate simplifying assumptions that limit their ranges of validity. To build on these methods, we develop a ``three-temperature" numerical scheme, which self-consistently models energy exchange between gas, dust, and radiation, as a part of the PLUTO radiation-hydrodynamics code. With a range of test problems in 0D, 1D, 2D, and 3D, we demonstrate the efficacy of our method, and make the case for its applicability to a wide range of problems in disk physics, including hydrodynamic instabilities and disk-planet interaction.

arXiv commentAccepted to Astronomy and Astrophysics; 16 pages, 11 figures incl. Appendix. Comments and questions welcome

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Cited by in corpus (14)

• Dust Coagulation Reconciles Protoplanetary Disk Observations with the Vertical Shear Instability. I. Dust Coagulation and the VSI Dead Zone
• Vertical shear instability in two-moment radiation-hydrodynamical simulations of irradiated protoplanetary disks I. Angular momentum transport and turbulent heating
• Vertical shear instability in two-moment radiation-hydrodynamical simulations of irradiated protoplanetary disks II. Secondary instabilities and stability regions
• TriPoD: Tri-Population size distributions for Dust evolution. Coagulation in vertically integrated hydrodynamic simulations of protoplanetary disks
• Three-temperature radiation hydrodynamics with PLUTO: Thermal and kinematic signatures of accreting protoplanets
• Can gap-edge illumination excite spirals in protoplanetary disks? Three-temperature radiation hydrodynamics and NIR image modelling
• Vertical shear instability with dust evolution and consistent cooling times. On the importance of the initial dust distribution
• Multidimensional half-moment multigroup radiative transfer. Improving moment-based thermal models of circumstellar disks
• The role of detailed gas and dust opacities in shaping the evolution of the inner disc edge subject to episodic accretion
• Monte Carlo post-processing for radiation hydro simulations of accreting planets in protoplanetary disks
• A new multifluid method for dusty astrophysical flows. Application to turbulent protostellar collapses
• Starlight-driven flared-staircase geometry in radiation hydrodynamic models of protoplanetary disks
• Modelling shadows in scattered light observations as signals from companions in protoplanetary discs
• Gas dynamics around dust asymmetries in turbulent disks