A5062227439- Stellar, planetary, and galactic studies
- Astrophysics and Star Formation Studies
- Astro and Planetary Science
- Molecular Spectroscopy and Structure
- Astronomy and Astrophysical Research
- Advanced Combustion Engine Technologies
- Galaxies: Formation, Evolution, Phenomena
- Computational Physics and Python Applications
- Legal and Regulatory Analysis
- Gamma-ray bursts and supernovae
- Arctic and Russian Policy Studies
- Distributed and Parallel Computing Systems
- Spacecraft and Cryogenic Technologies
- SAS software applications and methods
- Economic and Technological Developments in Russia
- Pulsars and Gravitational Waves Research
- Simulation Techniques and Applications
Leiden University
2019-2024
Leiden Observatory
2024
Planet-forming circumstellar disks are a fundamental part of the star formation process. Since stars form in hierarchical fashion groups up to hundreds or thousands, UV radiation environment that these exposed can vary strength by at least six orders magnitude. This limit masses and sizes disks. Diversity forming environments have long lasting effects disk evolution resulting planetary populations. We perform simulations explore young clusters. include viscous evolution, as well impact...
Abstract Feedback from massive stars plays an important role in the formation of star clusters. Whether a very is born early or late cluster timeline has profound implications for and assembly processes. We carry out controlled experiment to characterize effects early-forming on formation. use software suite Torch , combining self-gravitating magnetohydrodynamics, ray-tracing radiative transfer, N -body dynamics, stellar feedback, model four initially identical 10 4 M ⊙ giant molecular...
The mode of star formation that results in the globular clusters and young massive is difficult to constrain through observations. We present models cluster using T ORCH framework, which uses Astrophysical MUltipurpose Software Environment (AMUSE) couple distinct multi-physics codes handle formation, stellar evolution dynamics, radiative transfer, magnetohydrodynamics. upgraded by implementing N-body code P ETAR , thereby enabling forming from 10 6 M ⊙ clouds with ≥10 5 individual stars....
Protoplanetary discs spend their lives in the dense environment of a star forming region. While there, they can be affected by nearby stars through external photoevaporation and dynamic truncations. We present simulations that use AMUSE framework to couple Torch model for cluster formation from molecular cloud with evolution protoplanetary under these two environmental processes. compare without extinction photoevaporation-driving radiation. find majority our are considerably shielded...
We perform simulations of star cluster formation to investigate the morphological evolution embedded clusters in earliest stages their evolution. conduct our with Torch, which uses AMUSE framework couple state-of-the-art stellar dynamics formation, radiation, winds, and hydrodynamics FLASH. simulate a suite $10^4$ M$_{\odot}$ clouds at 0.0683 pc resolution for $\sim$ 2 Myr after onset virial parameters $\alpha$ = 0.8, 2.0, 4.0 different random samplings initial mass function prescriptions...
Circumstellar discs are the precursors of planetary systems and develop shortly after their host star has formed. In early stages these immersed in an environment rich gas neighbouring stars, which can be hostile for survival. There several environmental processes that affect evolution circumstellar discs, external photoevaporation is arguably one most important ones. Theoretical observational evidence point to losing mass quickly when vicinity massive, bright stars. this work we simulate...
The evolution of circumstellar discs is influenced by their surroundings. relevant processes include external photoevaporation due to nearby stars, and dynamical truncations. impact these on disc populations depends the star-formation history region. Since star formation phase-space characteristics stars are important for discs, we start simulating cluster with results molecular cloud collapse simulations. In simulation form which can be affected different processes. Our models account...
The Laser Interferometer Space Antenna (LISA) will enable Galactic gravitational wave (GW) astronomy by individually resolving $ > 10^4$ signals from double white dwarf (DWD) binaries throughout the Milky Way. In this work we assess for first time potential of LISA data to map stellar bar and spiral arms, since GWs are unaffected crowding dust extinction unlike optical observations bulge region. To achieve goal combine a realistic population DWDs with high-resolution N-Body simulation galaxy...
ABSTRACT Recently, several accreting M dwarf stars have been discovered with ages far exceeding the typical protoplanetary disc lifetime. These ‘Peter Pan discs’ can be explained as primordial discs that evolve in a low-radiation environment. The persistently low masses of host raise question whether survive up to these around higher mass. In this work we explore way which different mass loss processes limit their maximum lifetimes, and how depends on star We find ≲0.6 M⊙ retain for ∼50 Myr....
Context: Current exoplanet formation studies tend to overlook the birth environment of stars in clustered environments. The effect this on planet-formation process, however, is important, especially earliest stage. Aims: We investigate differences planet populations forming star-cluster environments through pebble accretion and compare these results with around isolated stars. try provide potential signatures young planetary systems guide future observation. Methods: design present a new...
Context. We present V ENICE , an operator-splitting algorithm to integrate a numerical model on hierarchy of timescales. Aims. allows wide variety different physical processes operating scales be coupled individual and adaptive time-steps. It therewith mediates the development complex multi-scale multi-physics simulation environments with independent components. Methods. The coupling between various models is dynamic, realised through (Strang) operators splitting using Results. demonstrate...
Abstract We simulate mergers between star clusters embedded within their natal giant molecular cloud. extract initial conditions from cloud-scale simulations of cluster formation and introduce different prescriptions for primordial binaries. find that do not include binaries result in a larger fraction unbound stars than prescription based on observations. also preferred direction motion become during the merger. Subcluster realistic gas environments promote binary disruption, while...
Some HII regions that surround young stellar clusters are bordered by molecular shells appear to expand at a rate inconsistent with our current model simulations. In this study we focus on the dynamics of Sharpless 171 (including NGC 7822), which surrounds cluster Berkeley 59. We aim compare velocity pattern over shell mean radial for estimates expansion velocities different structures, and match observed properties Optical spectra 27 stars located in 59 were collected Nordic Telescope,...
Context . Current exoplanet formation studies tend to overlook the birth environment of stars in clustered environments. However, effects this on planet process are important, especially earliest stage. Aims We investigate differences populations forming star-cluster environments through pebble accretion and compare these results with around isolated stars. strive provide potential signatures young planetary systems guide future observations. Methods present a new population synthesis code...
Feedback from massive stars plays an important role in the formation of star clusters. Whether a very is born early or late cluster timeline has profound implications for and assembly processes. We carry out controlled experiment to characterize effects early-forming on formation. use software suite \texttt{Torch}, combining self-gravitating magnetohydrodynamics, ray-tracing radiative transfer, $N$-body dynamics, stellar feedback model four initially identical $10^4$ M$_\odot$ giant...
Protoplanetary discs spend their lives in the dense environment of a star forming region. While there, they can be affected by nearby stars through external photoevaporation and dynamic truncations. We present simulations that use AMUSE framework to couple Torch model for cluster formation from molecular cloud with evolution protoplanetary under these two environmental processes. compare without extinction photoevaporation-driving radiation. find majority our are considerably shielded...
We perform simulations of star cluster formation to investigate the morphological evolution embedded clusters in earliest stages their evolution. conduct our with Torch, which uses AMUSE framework couple state-of-the-art stellar dynamics formation, radiation, winds, and hydrodynamics FLASH. simulate a suite $10^4$ M$_{\odot}$ clouds at 0.0683 pc resolution for $\sim$ 2 Myr after onset virial parameters $α$ = 0.8, 2.0, 4.0 different random samplings initial mass function prescriptions...
The mode of star formation that results in the globular clusters and young massive is difficult to constrain through observations. We present models cluster using Torch framework, which uses AMUSE couple distinct multi-physics codes handle formation, stellar evolution dynamics, radiative transfer, magnetohydrodynamics. upgrade by implementing N-body code PeTar, thereby enabling forming from $10^6\rm\, M_\odot$ clouds with $\ge10^5$ individual stars. simulations $10^4, 10^5$, $10^6\rm...
Abstract Stars form in clusters, while planets gaseous disks around young stars. Cluster dissolution occurs on longer time scales than disk dispersal. Planet formation thus typically takes place the host star is still inside cluster. We explore how presence of other stars affects evolution circumstellar disks. Our numerical approach requires multi-scale and multi-physics simulations where relevant components their interactions are resolved. The start with collapse a turbulent cloud, from...