Aurorae are well known optical phenomena in the Solar System planets. Aurorae have great diagnostic value, as their emissions reveal the planets’ atmospheric compositions, the occurrence of magnetic fields and the solar wind conditions at the planet’s orbit. Looking for aurorae on exoplanets and brown dwarfs is the next frontier. A first breakthrough in this direction has occurred recently, with the detection of a CH4 emission attributed to auroral excitation on the brown dwarf W1935. This detection, and the prospects of observing other auroral features with existent and upcoming telescopes, is what motivates this project. In particular, we will build the first model dedicated to investigate CH4 and H3+ auroral emission on exoplanets and brown dwarfs. The model will be used to investigate the conditions at W1935, and to predict the detectability of aurorae on other sub-stellar objects.
Beam dynamics for a multi-stage laser-plasma accelerator
Laser–plasma wakefield accelerators (LWFAs) can provide accelerating gradients exceeding 100 GV/m, providing a pathway to reduce the size and cost of future high-energy accelerators for applications in synchrotron radiation, free-electron lasers, and emerging medical and industrial uses.
Scaling this technology to higher beam energies and charges requires both technological maturity and innovative acceleration schemes. Multi-stage configurations — connecting several plasma acceleration stages — offer key advantages: increasing beam energy beyond single-cell limits and enhancing total charge and/or repetition rate. These systems aim to overcome single-stage limitations while maintaining or improving beam quality at higher energies.
Designing an accelerator delivering stable, reproducible, high-quality beams requires comprehensive understanding of plasma acceleration physics and beam transport between successive stages.
Building on expertise at CEA Paris–Saclay's DACM, this PhD will focus on physical and numerical studies to propose a fully integrated multi-stage LWFA design, with particular attention to optimizing all components — plasma accelerating section and transport lines — to preserve beam quality in terms of transverse size, divergence, emittance, and energy spread.
Exploring trends in rocky exoplanets observed with JWST
One of JWST’s major goals is to characterize, for the first time, the atmospheres of rocky, temperate exoplanets, a key milestone in the search for potentially habitable worlds. The temperate rocky exoplanets accessible to JWST are primarily those orbiting M-type stars. However, a major question remains regarding the ability of planets orbiting M-dwarfs to retain their atmospheres.
In 2024, an exceptional 500-hour Director’s Discretionary Time (DDT) program, entitled Rocky Worlds, was dedicated to this topic, underlining its strategic importance at the highest level (NASA, STScI).
The main objective of this PhD project is to: 1) Analyze all available JWST/MIRI eclipse data for rocky exoplanets from Rocky Worlds and other public programs using a consistent and homogeneous framework; 2)Search for population-level trends in the observations and interpret them using 3D atmospheric simulations.
Through this work, we aim to identify the physical processes that control the presence and composition of atmospheres on temperate rocky exoplanets.
Stochastic Neutron Noise Estimation Using a Rare-Event Simulation Approach. Application to the Monitoring of Nuclear System Reactivity
This PhD project aims to develop an innovative method to characterize the reactivity of fissile systems by analyzing their stochastic fluctuations, known as zero-power neutron noise. In a subcritical fissile medium, neutrons originating from spontaneous fission can initiate short and random chain reactions, generating a fluctuating signal. This noise carries essential information on the distance of the system to criticality, a key parameter both for the safety of nuclear installations (prevention of criticality accidents) and for the detection of undeclared fissile materials (nuclear security and non-proliferation).
Existing theoretical approaches to infer system reactivity from neutron noise are limited to idealized situations and become unsuitable in realistic configurations, particularly when the system is strongly subcritical or when significant uncertainties exist regarding its geometry or composition (as in the case of the Fukushima Daiichi corium or spent fuel storage). Monte Carlo simulations then appear as a natural alternative, but current simulations rely on variance reduction techniques that fail to correctly preserve stochastic fluctuations.
This thesis proposes to address this scientific challenge by adapting a relatively recent variance reduction method known as Adaptive Multilevel Splitting (AMS), originally developed to efficiently sample rare events while preserving their statistical properties. The goal is to extend this method to neutron transport in multiplying media and to make it a tool capable of faithfully simulating the temporal correlations characteristic of neutron noise. Following the theoretical developments, the algorithm will be implemented in Geant4, compared to analytical benchmark solutions, and experimentally validated through in situ measurements (using neutron sources or research reactors). In the long term, this work may lead to direct applications in nuclear monitoring, safety diagnostics, and detector physics, while also opening perspectives in fundamental physics and medical physics.
Magnetar formation: from amplification to relaxation of the most extreme magnetic fields
Magnetars are neutron stars with the strongest magnetic fields known in the Universe, observed as high-energy galactic sources. The formation of these objects is one of the most studied scenarios to explain some of the most violent explosions: superluminous supernovae, hypernovae, and gamma-ray bursts. In recent years, our team has succeeded in numerically reproducing magnetic fields of magnetar-like intensities by simulating dynamo amplification mechanisms that develop in the proto-neutron star during the first seconds after the collapse of the progenitor core. However, most observational manifestations of magnetars require the magnetic field to survive over much longer timescales (from a few weeks for super-luminous supernovae to thousands of years for Galactic magnetars). This thesis will consist of developing 3D numerical simulations of magnetic field relaxation initialized from different dynamo states previously calculated by the team, extending them to later stages after the birth of the neutron star when the dynamo is no longer active. The student will thus determine how the turbulent magnetic field generated in the first few seconds will evolve to eventually reach a stable equilibrium state, whose topology will be characterized and compared with observations.
Understanding the origin of the remarkable efficiency of distant galaxy formation
The James Webb Space Telescope is revolutionizing our understanding of the distant universe. A result has emerged that challenges our models: the extremely high efficiency of star formation in distant galaxies. However, this finding is derived indirectly: we measure the mass of stars in galaxies, not their star formation rate. This is the main weakness of the James Webb. The aim of this thesis is to remedy this weakness by using its angular resolution capacity, which has not been taken into account until now, in order to obtain a more robust measurement of the SFR of distant galaxies. We will deduce a law that will improve the robustness of SFR determination using morphological properties and combining data from the James Webb Space Telescope with data from ALMA (z=1-3). We will then apply it to the distant universe (z=3-6, part 2) and use it as a benchmark for numerical simulations (part 3).
Spectro-temporal analysis of Gamma-Ray Burst afterglows detected with SVOM
Gamma-Ray Bursts (GRB) are the most powerful explosions in the Universe. They last a few tens of seconds and emit the same amount of energy as the Sun during its entire lifetime. They gamma-ray emission is followed by a long lasting (hours to days) emission from the X-rays to the radio band. This "afterglow" emission is rich on information about the GRB nearby environnent and host galaxy. SVOM (Space based astronomical Variable Object Monitor) is a Sino-French mission, dedicated to GRB studies, and has been successfully launched in June 2024. It carries a multi-wavelength payload covering gamma-rays/X-rays/optical and includes two dedicated ground based robotic telescopes in Mexico and China.
The PHD project is focussed on the exploitation of the SVOM data for GRBs. The successful candidate will join the MXT science Teal at DAp. MXT is a new type of X-ray telescope, for which the DAp is responsible and its Instrument Centre is also hosted at DAp.
The PHD student will participate actively to the spectral and temporal analysis of MXT data. These data will be compared
to the other data acquired by the SVOM collaboration, especially in the optical an infrared domains.
This dataset will be used as a support to the physical interpretation of GRBs. More specifically, the aspects related to the modeling of the energy injection in the first phases of the afterglow will be used to determine the nature of the compact object at the origin of the relativistic flux, generating the electromagnetic emission observed.
Exotic shape of the nucleus: decay spectroscopy of neutron-deficient actinides with the detector SEASON
The question of the limit of stability of nuclei, both in terms of proton/neutron asymmetry and in terms of mass, is an important open question in modern nuclear physics. In the region of heavy nuclei, the neutron-deficient actinides present a great interest. Indeed, strong octupolar deformation, giving a pear shape to the nuclei, are predicted and have event been already observed in some isotopes. These deformations seem to play a key role for nuclear stability, for nuclear decay modes, and may also be related to physics beyond the standard model. The main goal oh this thesis will be to pursue the systematic study of these deformations by making use of the brand-new SEASON detector, whose first experiment will take place at the University of Jyväskylä (Finland) in February 2026. The thesis will focus on the analysis of data from the experimental campaign that will occur in summer 2026. Several experiments are foreseen, making use of different beam-target combinations to produce actinides by fusion-evaporation reaction. These actinides will then be sent inside SEASON to perform their decay spectroscopy. Depending on the plannings, another campaign could be scheduled at Jyväskylä in 2027. Finally, the return of the instrument in France to be set up at GANIL-Spiral2 (Caen) coupled to the S3 spectrometer will certainly take place this the thesis period.
The thesis can be co-directed by the university of Jyväskylä.
TRANSFORMER: from the genealogy of dark matter halos to the baryonic properties of galaxy clusters.
The thesis proposes to predict the baryonic properties of galaxy clusters based on the history of dark matter halo formation, using innovative neural networks (Transformers). The work will involve intensive numerical simulations. This project falls within the general framework of determining cosmological parameters through the observation of galaxy clusters in X-rays. It is directly linked to the international Heritage programme in the XMM-Euclid FornaX deep field.
Machine Learning-Based Algorithms for Real-Time Standalone Tracking in the Upstream Pixel Detector at LHCb
This PhD aims to develop and optimize next-generation track reconstruction capabilities for the LHCb experiment at the Large Hadron Collider (LHC) through the exploration of advanced machine learning (ML) algorithms. The newly installed Upstream Pixel (UP) detector, located upstream of the LHCb magnet, will play a crucial role from Run 5 onward by rapidly identifying track candidates and reducing fake tracks at the earliest stages of reconstruction, particularly in high-occupancy environments.
Achieving fast and highly efficient tracking is essential to fulfill LHCb’s rich physics program, which spans rare decays, CP-violation studies in the Standard Model, and the characterization of the quark–gluon plasma in nucleus–nucleus collisions. However, the increasing event rates and data complexity expected for future data-taking phases will impose major constraints on current tracking algorithms, especially in heavy-ion collisions where thousands of charged particles may be produced per event.
In this context, we will investigate modern ML-based approaches for standalone tracking in the UP detector. Successful applications in the LHCb VELO tracking system already demonstrate the potential of such methods. In particular, Graph Neural Networks (GNNs) are a promising solution for exploiting the geometric correlations between detector hits, allowing for improved tracking efficiency and fake-rate suppression, while maintaining scalability at high multiplicity.
The PhD program will first focus on the development of a realistic GEANT4 simulation of the UP detector to generate ML-suitable datasets and study detector performance. The next phase will consist in designing, training, and benchmarking advanced ML algorithms for standalone tracking, followed by their optimization for real-time GPU-based execution within the Allen trigger and reconstruction framework. The most efficient solutions will be integrated and validated inside the official LHCb software stack, ensuring compatibility with existing data pipelines and direct applicability to Run-5 operation.
Overall, the thesis will provide a major contribution to the real-time reconstruction performance of LHCb, preparing the experiment for the challenges of future high-luminosity and heavy-ion running.