Monte Carlo post-processing for radiation hydro simulations of accreting planets in protoplanetary disks
arXiv:2501.14858 · doi:10.1051/0004-6361/202451780
Abstract
This paper is part of a series investigating the observational appearance of planets accreting from their nascent protoplanetary disk (PPD). We evaluate the differences between gas temperature distributions determined in our radiation hydrodynamical (RHD) simulations and those recalculated via post-processing with a Monte Carlo (MC) radiative transport (RT) scheme. Our MCRT simulations were performed for global PPD models, each composed of a local 3D high-resolution RHD model embedded in an axisymmetric global disk simulation. We report the level of agreement between the two approaches and point out several caveats that prevent a perfect match between the temperature distributions with our respective methods of choice. Overall, the level of agreement is high, with a typical discrepancy between the RHD and MCRT temperatures of the high-resolution region of only about 10 percent. The largest differences were found close to the disk photosphere, at the transition layer between optically dense and thin regions, as well as in the far-out regions of the PPD, occasionally exceeding values of 40 percent. We identify several reasons for these discrepancies, which are mostly related to general features of typical radiative transfer solvers used in hydrodynamical simulations (angle- and frequency-averaging and ignored scattering) and MCRT methods (ignored internal energy advection and compression and expansion work). This provides a clear pathway to reduce systematic temperature inaccuracies in future works. Based on MCRT simulations, we finally determined the expected error in flux estimates, both for the entire PPD and for planets accreting gas from their ambient disk, independently of the amount of gas piling up in the Hill sphere and the used model resolution.
Accepted for publication in A&A, 31 pages, 28 figures, 2 tables
References in corpus (12)
- The Near-Infrared Spectrograph (NIRSpec) on the James Webb Space Telescope I. Overview of the instrument and its capabilities
- Two accreting protoplanets around the young star PDS 70
- A comparative study of disc-planet interaction
- Images of Embedded Jovian Planet Formation At A Wide Separation Around AB Aurigae
- The newborn planet population emerging from ring-like structures in discs
- VLT/SPHERE exploration of the young multiplanetary system PDS70
- An Implicit Finite Volume Scheme to Solve the Time Dependent Radiation Transport Equation Based on Discrete Ordinates
- Tracing large-scale structures in circumstellar disks with ALMA
- Tracing planet-induced structures in circumstellar disks using molecular lines
- Self-consistent dust and non-LTE line radiative transfer with SKIRT
- Three-temperature radiation hydrodynamics with PLUTO: Tests and applications to protoplanetary disks
- The scattering order problem in Monte Carlo radiative transfer