Simulations of thermal surface waves in a protoplanetary disk using 1+1D approximation
arXiv:2203.06614 · doi:10.1134/S1063772922050055
Abstract
Heating by the central star is one of the key factors determining the physical structure of protoplanetary disks. Due to the large optical thickness in the radial direction, disk midplane regions are heated by the infrared radiation from the disk surface (atmosphere), which in turn is directly heated by the star. It was previously shown that interception of the stellar radiation by inhomogeneities on the disk surface can cause perturbations that propagate towards the star. In this work, we investigate the occurrence of such waves within a detailed 1+1D numerical model of the protoplanetary disk. We confirm the previous findings that in the disk, that is optically thick to its own radiation, the surface perturbations indeed occur and propagate towards the star. However, contrary to some analytical predictions, the thermal waves in sufficiently massive disks affect only the upper layers without significant fluctuations of temperature in the midplane. Our results indicate the need to study this instability within more consistent hydrodynamic models.
arXiv commentAccepted for publication in Astronomy Reports (2022)
References in corpus (14)
- Streaming Instabilities in Protoplanetary Disks
- First Results from High Angular Resolution ALMA Observations Toward the HL Tau Region
- The Disk Substructures at High Angular Resolution Project (DSHARP): II. Characteristics of Annular Substructures
- Observations of Protoplanetary Disk Structures
- The Disk Substructures at High Angular Resolution Project (DSHARP): VII. The Planet-Disk Interactions Interpretation
- Observational Signatures of Planets in Protoplanetary Disks I: Gaps Opened by Single and Multiple Young Planets in Disks
- On the formation of multiple concentric rings and gaps in protoplanetary disks
- Two mechanisms for dust gap opening in protoplanetary discs
- Thermal Waves in Irradiated Protoplanetary Disks
- Thermal Wave Instability as an Origin of Gap and Ring Structures in Protoplanetary Disks
- Shadows, gaps, and ring-like structures in protoplanetary disks
- Improving the thin-disk models of circumstellar disk evolution. The 2+1-dimensional model
- Evolution of a Viscous Protoplanetary Disk with Convectively Unstable Regions
- Evolution of a Viscous Protoplanetary Disk with Convectively Unstable Regions. II. Accretion Regimes and Long-Term Dynamics