Welcome to my homepage!

I am a PhD student at the Institute of Astronomy, Charles University in Prague.
My primary interest is the theory of planet formation, hydrodynamical evolution of protoplanetary disks
and planet-disk interactions. This website provides an overview of my current research as well as
previously published papers, meeting contributions and source codes available for the community.

The FARGO_THORIN hydrocode

FARGO_THORIN (or THORIN for short) stands for FARGO with Two-fluid HydrOdynamics, the Rebound integrator Interface and Non-isothermal gas physics. The program is an extension of the standard 2D FARGO code (Masset 2000). The code features are briefly described below, see also Chrenko et al. (2017) for a thorough description of the implemented physics.

The code is publicly available under the terms of this license (see also the GNU General Public License ).
Latest version: Jul 6 2017; first public release (v 1.0)


Highlights from my recent paper:

Left: Gas temperature in the vicinity of a super-Earth which is heated by pebble accretion and illuminates its surroundings (the circle represents the Hill sphere). The overheated gas forms a hot trail behind the embryo. Right: Evolution of four super-Earths migrating in the disk with accretion heating accounted for.

Evolution of protoplanets growing by pebble accretion

According to recent developments in the planet formation theory, protoplanets form by accretion of small solid particles, known as pebbles, which move through the gaseous media and are decelerated by the aerodynamic drag. Owing to the vigorous material deposition, protoplanets grow rapidly, they become heated and radiate the excessive energy into their surroundings. At the same time, protoplanets migrate due to gravitational interactions with the surrounding disk. I study the evolution of newborn planetary systems while taking into account all the aforementioned phenomena simultaneously, thus providing a realistic feedback between all the system components. Hydrodynamic global-scale simulations are necessary for this purpose.

Closeup of the surface density in an evolving protoplanetary disk consisting of the gas (left) and pebble component (right), interacting with embedded super-Earths.

Two-fluid hydrodynamic code with pebble accretion

I have developed an extension of the 2D FARGO hydrocode. The additional features:

  • Non-isothermal gas disk with the internal energy equation accounting for compressional heating, viscous friction, in-plane radiative diffusion, vertical radiation escape, stellar irradiation and accretion heating.
  • Pebble disk treated as an Eulerian pressureless and inviscid fluid, coupled with the gas disk through the Epstein drag term. Massive bodies accrete from the pebble component self-consistently.
  • Rebound package interface allowing for e.g. 3D high-order orbital integration with adaptive time-stepping (IAS15 integrator), collision search, etc.
  • Gravitational planet-disk interaction calculated by means of a vertically-averaged potential assuming a simple vertical distribution of gas (and pebbles) over the corresponding scale height.

For a detailed code description, see Chrenko et al. (2017).
You can get your own copy of the code on this website!


Meeting contributions

  • AAS DPS 2017 - Evolution of migrating protoplanets heated by pebble accretion (talk): ADS entry
  • AAS DPS/EPSC 2016 - Building the giant planet cores by convergent migration of pebble-accreting embryos (poster): ADS entry, download pdf
  • AAS DPS 2015 - Planetesimals embedded in a gaseous disc vs mean-motion resonances (poster): ADS entry, download pdf
  • AAS DPS 2014 - The origin of the long-lived asteroids in the 2:1 mean-motion resonance with Jupiter (talk): ADS entry


Websites which might interest you

  • Homepage of my PhD supervisor and collaborator Miroslav Brož
  • Research of minor solar-system bodies at Charles University: Yarko-site devoted to general dynamics & SPH collisions; DAMIT database of the asteroid shape models derived from light curve inversions