A5023459977- Astrophysics and Star Formation Studies
- Stellar, planetary, and galactic studies
- Astrophysical Phenomena and Observations
- Image Processing and 3D Reconstruction
- Plant Water Relations and Carbon Dynamics
- 3D Shape Modeling and Analysis
- Computer Graphics and Visualization Techniques
- Space Exploration and Technology
- Astro and Planetary Science
- Pulsars and Gravitational Waves Research
- Fluid Dynamics and Turbulent Flows
Heidelberg University
2019-2021
Heidelberg Institute for Theoretical Studies
2021
Planetary migration is a key link between planet formation models and observed exoplanet statistics. So far the theory of has focused on interaction planets with an inviscid or viscously evolving disk. Turbulent viscosity thought to be main driver disk evolution known affect process. Recently, topic wind-driven accretion experiencing renaissance, as evidence mounting that PPDs may less turbulent than previously thought, 3-D non-ideal MHD modeling wind-launching process maturing. Aim: We wish...
Context. Multiple observations have offered evidence that a significant fraction of protoplanetary disks contain warps. A warp in disk evolves over time, affecting the appearance and shape shadows arcs. It also greatly influences kinematic signatures. Understanding evolution helps provide valuable insights into its origins. Aims. Thus far, numerous theoretical studies warped been conducted using methods based on smoothed particle hydrodynamics (SPH). In our approach, we use grid-based method...
The dynamical interactions between young binaries can perturb the material distribution of their circumstellar disks, and modify planet formation process. In order to understand how planets form in multiple stellar systems, it is necessary characterize both binary orbit disks properties. constrain impact nature interaction RW\,Aur system (bound or unbound), we analyzed at 1.3\,mm wavelengths, as observed epochs by Atacama Large (sub-)millimeter Array (ALMA). We disk properties through...
The 1-D evolution equations for warped discs come in two flavors: For very viscous the internal torque vector G is uniquely determined by local conditions disc, and warps tend to damp out rapidly if they are not continuously driven. inviscid discs, on other hand, becomes a dynamic quantity, warp will propagate through disc as wave. governing both regimes usually treated separately. A unified set of was postulated recently Martin et al. (2019), but yet derived from underlying physics....
Observations show evidence that a significant fraction of protoplanetary disks contain warps. A warp in disk evolves time affecting the appearance shadows and greatly influencing kinematic signatures. So far, many theoretical studies warped have been conducted using Smoothed Particle Hydrodynamics (SPH) methods. In our approach, we use grid-based method spherical coordinates which has notable advantages: allows for accurate modelling low viscosity values resolution does not depend on density...
The dynamical interactions between young binaries can perturb the material distribution of their circumstellar disks, and modify planet formation process. In order to constrain impact nature binary interaction in RW Aur system (bound or unbound), we analyzed at 1.3 mm wavelengths, as observed multiple epochs by ALMA. We disk properties through parametric visibility modeling, used this information dust morphology orbital period. imaged continuum emission with a resolution 3 au, find that...