Title of HDR
Cool evolved stars feedback at high angular resolution.
Composition of the jury
- Ana Palacios, Rapportrice, Observatoire de Recherche Montpelliérain de l’Environnement
- Céline Reylé, Rapportrice, Observatoire des Sciences de l’Univers Terre Homme Environnement Temps Astronomie
- Philippe Stee, Rapporteur, Observatoire de la Côte d’Azur
- Vincent Coudé du Foresto, Examinateur, Observatoire de Paris - PSL
- Fabien Baron, Examinateur, Georgia State University
- Alex de Koter, Examinateur, Anton Pannekoek Institute for Astronomy
Summary
To understand the ultimate evolution phase of stars – at the origin of compact objects, the chemical enrichment of the Universe and the elementary building blocks of future exoplanets – it is essential to characterise their mass loss during the cool evolved stages. It plays a crucial role in determining the final mass of stars, and in the growth of the cocoon of gas and dust at the origin of future planetary nebulæ (low-mass or intermediate-mass stars), or which will determine our perception of supernova explosions (massive stars).
My research covers three main areas : the origin of mass loss of red supergiant stars, the mechanisms shaping the stellar wind of stars on the asymptotic giant branch, and the formation of dust in the environment of these two types of star. To do this, I use observations in optical interferometry, adaptive optics and polarisation in visible light, and millimetre interferometry. These observations are analysed using analytical models and numerical hydrodynamics radiative and 3D radiative transfer simulations.
In the future, this field will benefit from major advances in terms of instrumentation (ELT, Vera Rubin Observatory, future interferometers), which will allow resolving unprecedented structures of evolved stars and their environment.
