Akumulace prachu ve 2D protoplanetárních discích s viskózním ohřevem
| Thesis title in Czech: | Akumulace prachu ve 2D protoplanetárních discích s viskózním ohřevem |
|---|---|
| Thesis title in English: | Dust accumulation in 2D protoplanetary disks with viscous heating |
| Academic year of topic announcement: | 2025/2026 |
| Thesis type: | diploma thesis |
| Thesis language: | |
| Department: | Astronomical Institute of Charles University (32-AUUK) |
| Supervisor: | RNDr. Ondřej Chrenko, Ph.D. |
| Author: | |
| Advisors: | doc. Mgr. Miroslav Brož, Ph.D. |
| Guidelines |
| Recent advances in planet formation theory suggest that, in order to grow dust into planetesimals, the dust-to-gas ratio in a protoplanetary disk must increase locally to enable the streaming instability and/or direct gravitational collapse (Birnstiel et al. 2016; Drążkowska et al. 2023). Dust accumulations, observed for instance as ring-like structures with ALMA, can be facilitated by local gas pressure maxima, often referred to as pressure bumps. Yet, the physical origin of such bumps remains uncertain.
Kato et al. (2025) have proposed a one-dimensional model in which pressure bumps arise self-consistently from the feedback between dust concentration and viscous heating. In this scenario, an overdense dust perturbation leads to a local temperature increase, as the disk cools less efficiently. This can trigger a positive feedback loop that produces a temperature-driven pressure bump in the gas, capable of trapping additional dust. The primary aim of this thesis is to extend the work of Kato et al. (2025) by developing a more sophisticated two-dimensional (radius-azimuth) model of a gas-dust disk. The student will first familiarize themselves with the public hydrodynamic code Fargo3D (Benítez-Llambay & Masset 2016), initially in its locally isothermal setup, and learn how to run multi-fluid gas-dust simulations with aerodynamic drag. Subsequently, the student will consider more realistic disk thermodynamics, including at least viscous heating and radiative cooling from the disk surfaces (e.g. Chrenko et al. 2017). The radiative cooling rate will be implemented using a self-consistent relation between the local dust concentration, grain size, and the resulting optical depth. After an initial exploration of the parameter space (primarily viscosity and grain size), the student may increase the model’s realism by incorporating dust coagulation (Drążkowska et al. 2019; Pfeil et al. 2024) or by studying the effects of dust sublimation lines relevant to inner disk regions. The student will learn how to work in Linux, how to program in C and Python, and how to apply parallelization techniques such as OpenMP/MPI/CUDA. The student will learn how to access and utilize available high-performance computing centres such as the faculty cluster Chimera, MetaCentrum, or IT4Innovations. |
| References |
| Benítez-Llambay, P. & Masset, F. S. 2016, ApJS, 223, 11B
Birnstiel, T. et al. 2016, SSRv, 205, 41B Chrenko, O. et al. 2017, A&A, 606A, 114C Drazkowska, J. et al. 2019, ApJ, 885, 91D Drazkowska, J. et al. 2023, ASPC, 534, 717D Kato, R. et al. 2025, PASJ, 77, 718D Pfeil, T. et al. 2024, A&A, 691A, 45P |