Sébastien Martinet

Doctorant

311
+41 22 379 24 55
Courriel

Direction de thèse: Prof. Georges Meynet et Dr. Sylvia Ekström.

L'évolution des étoiles les plus massives au cours de l'histoire de l'Univers.

Mes recherches se portent sur l'évolution stellaire des étoiles massives, en utilisant le code GENEC, développé ici à Genève. Mon principal axe de recherche se porte sur l'évolution des étoiles les plus massives. Ces étoiles ne sont pas que des objets spectaculaires, mais elles ont aussi un impact considérable sur leur environnement, et à plus grande échelle sur l'Univers. La nucléosynthèse durant leur vie, mais aussi lors de leur explosion finale en supernova, contribue largement à l'enrichissement global de l'Univers. De plus, les conditions extrêmes à la surface et à l'intérieur de ces étoiles engendrent des effets radiatifs et dynamiques très importants, tant localement qu'à l'échelle de l'Univers.

Papier récent: Martinet et al. 2021 (2021A&A...648A.126M)

Membres

Convective core sizes in rotating massive stars. I. Constraints from solar metallicity OB field stars

Combining stellar evolution models and spectroscopic parameters derived for a large sample of Galactic O and B stars with the inclusion of brand-new information about their projected rotational velocities, we reexamine the question of the convective core size in MS massive stars.

Ionizing photon production of Population III stars: effects of rotation, convection, and initial mass function

This work presents ionizing photon production predictions for the most up to date Geneva stellar evolution models of Population III stars, and provides insight into how key evolutionary parameters impact the contribution of the first stars to reionization.

Grids of stellar models with rotation - V. Models from 1.7 to 120 M⊙ at zero metallicity

Here we compute a grid of stellar evolution models using the Geneva code with the aim to improve our understanding of the evolution of zero-metallicity stars, with particular interest in how rotation affects surface properties, interior structure, and metal enrichment. We produce a range of models of initial masses (Mini) from 1.7 to 120M⊙ , focusing on massive models of 9≤Mini≤120M⊙ .

Grids of stellar models with rotation. VI. Models from 0.8 to 120 M⊙ at a metallicity Z = 0.006

The present models are of particular interest for comparisons with observations in the LMC and also in the outer regions of the Milky Way. We provide public access to numerical tables that can be used for computing interpolated tracks and for population synthesis studies.