A probabilistic numerical solver for initial value problems on ordinary differential equations. GitLab repository.
Robot Analysis Infrastructure
A framework to analyze synchronously sensors data and video captures of the scene from robotic experiments. GitLab repository.
MESA and NuGrid collaborations
NuGrid is a scientific collaboration studying nucleosynthesis in stellar interiors. As a member of this collaboration, I am developing and maintaining part of their workflow, in particular a HDF5 framework used with the open-source code MESA for flexible data handling. GitHub repository
Comparison of stellar evolution codes
A comparative study of several CFD codes modeling the life of stars. The main goal of this project was to better understand the intrinsic uncertainties of such techniques (see this paper).
Gravity solver for CFD codes
I developed and implemented a new algorithm to resolve gravitational effects more accurately in CFD simulations. The algorithm uses an adaptive particle-mesh technique (see this article).
Planets and stars
A study on the survivability of planets engulfed by their host star. This project led to several publications in general press (see the Press page).
An investigation the capabilities of CFD codes to model Kelvin-Helmoltz instabilities (see this article).
A project aiming at understanding the physical mechanisms in play when two stars merge, and trying to predict the outcome of this violent interaction. For this purpose, I developed parts of several CFD codes and performed 3D simulations of stellar mergers. Then I validated the simulations with observational data.
Le soleil, géante rouge, engloutit la planète
Interview pour le dossier mensuel "Demain la Terre".
66th Spring Conference of the German Ergonomics Society, 2020 (conference)
Unser digitales Zeitalter lebt von Informationen und stellt unsere begrenzte Verarbeitungskapazität damit täglich auf die Probe. Gerade in der Wissensarbeit haben ständige Ablenkungen erhebliche Leistungseinbußen zur Folge. Unsere intelligente Anwendung ACTrain setzt genau an dieser Stelle an und verwandelt Computertätigkeiten in eine Trainingshalle für den Geist. Feedback auf Basis maschineller Lernverfahren zeigt anschaulich den Wert auf, sich nicht von einer selbst gewählten Aufgabe ablenken zu lassen. Diese metakognitive Einsicht soll zum Durchhalten motivieren und das zugrunde liegende Fertigkeitsniveau der Aufmerksamkeitskontrolle stärken. In laufenden Feldexperimenten untersuchen wir die Frage, ob das Training mit diesem optimalen Feedback die Aufmerksamkeits- und Selbstkontrollfertigkeiten im Vergleich zu einer Kontrollgruppe ohne Feedback verbessern kann.
Monthly Notices of the Royal Astronomical Society, 477, June 2018 (article)
The common envelope binary interaction remains one of the least understood phases in the evolution of compact binaries, including those that result in Type Ia supernovae and in mergers that emit detectable gravitational waves. In this work, we continue the detailed and systematic analysis of 3D hydrodynamic simulations of the common envelope interaction aimed at understanding the reliability of the results. Our first set of simulations replicate the five simulations of Passy et al. (a 0.88 M☉, 90 R☉ red giant branch (RGB) primary with companions in the range 0.1-0.9 M☉) using a new adaptive mesh refinement gravity solver implemented on our modified version of the hydrodynamic code ENZO. Despite smaller final separations obtained, these more resolved simulations do not alter the nature of the conclusions that are drawn. We also carry out five identical simulations but with a 2.0 M☉ primary RGB star with the same core mass as the Passy et al. simulations, isolating the effect of the envelope binding energy. With a more bound envelope, all the companions in-spiral faster and deeper, though relatively less gas is unbound. Even at the highest resolution, the final separation attained by simulations with a heavier primary is similar to the size of the smoothed potential even if we account for the loss of some angular momentum by the simulation. As a result, we suggest that an ∼2.0 M☉ RGB primary may possibly end in a merger with companions as massive as 0.6 M☉, something that would not be deduced using analytical arguments based on energy conservation.
Iaconi, R., Reichardt, T., Staff, J., De Marco, O., Passy, J., Price, D., Wurster, J., Herwig, F.
Monthly Notices of the Royal Astronomical Society, 464, pages: 4028-4044, 2017 (article)
We present hydrodynamic simulations of the common envelope binary interaction between a giant star and a compact companion carried out with the adaptive mesh refinement code enzo and the smooth particle hydrodynamics code phantom. These simulations mimic the parameters of one of the simulations by Passy et al. but assess the impact of a larger, more realistic initial orbital separation on the simulation outcome. We conclude that for both codes the post-common envelope separation is somewhat larger and the amount of unbound mass slightly greater when the initial separation is wide enough that the giant does not yet overflow or just overflows its Roche lobe. phantom has been adapted to the common envelope problem here for the first time and a full comparison with enzo is presented, including an investigation of convergence as well as energy and angular momentum conservation. We also set our simulations in the context of past simulations. This comparison reveals that it is the expansion of the giant before rapid in-spiral and not spinning up of the star that causes a larger final separation. We also suggest that the large range in unbound mass for different simulations is difficult to explain and may have something to do with simulations that are not fully converged.
The common envelope (CE) binary interaction occurs when a star transfers mass onto a companion that cannot fully accrete it. The interaction can lead to a merger of the two objects or to a close binary. The CE interaction is the gateway of all evolved compact binaries, all stellar mergers, and likely many of the stellar transients witnessed to date. CE simulations are needed to understand this interaction and to interpret stars and binaries thought to be the byproduct of this stage. At this time, simulations are unable to reproduce the few observational data available and several ideas have been put forward to address their shortcomings. The need for more definitive simulation validation is pressing and is already being fulfilled by observations from time-domain surveys. In this article, we present an initial method and its implementation for post-processing grid-based CE simulations to produce the light curve so as to compare simulations with upcoming observations. Here we implemented a zeroth order method to calculate the light emitted from CE hydrodynamic simulations carried out with the 3D hydrodynamic code Enzo used in unigrid mode. The code implements an approach for the computation of luminosity in both optically thick and optically thin regimes and is tested using the first 135 days of the CE simulation of Passy et al., where a 0.8 M ⊙ red giant branch star interacts with a 0.6 M ⊙ companion. This code is used to highlight two large obstacles that need to be overcome before realistic light curves can be calculated. We explain the nature of these problems and the attempted solutions and approximations in full detail to enable the next step to be identified and implemented. We also discuss our simulation in relation to recent data of transients identified as CE interactions.
Our goal is to understand the principles of Perception, Action and Learning in autonomous systems that successfully interact with complex environments and to use this understanding to design future systems