Cinquième Assemblée Générale du GdR Ondes Gravitationnelles

Session

Groupe de Travail: Etoiles à neutrons, supernovae et synthèse des éléments lourds

12 oct. 2021, 13:00

LAPP - Laboratoire d'Annecy de Physique des Particules

24. Gravitational waves from core-collapse supernovae with strong rotation and magnetic fields

Dr Matteo Bugli (CEA - Saclay)

12/10/2021 13:00

ÉTOILES A NEUTRONS, SUPERNOVÆ ET SYNTHÈSES DES ÉLÉMENTS LOURDS

Core-collapse supernovae (CCSN) are an important formation channel for astrophysical compact objects that release huge quantities of gravitational binding energy in the form of neutrino emission, energetic ejecta and gravitational waves (GW).
The latter represent an extraordinary tool to probe the properties of the forming proto-neutron star (PNS), such as its mass and radius, and the...

9. Maximum mass of compact stars from gravitational wave events with finite-temperature equations of state

Micaela Oertel (LUTH, Observatoire de Paris)

12/10/2021 13:15

ÉTOILES A NEUTRONS, SUPERNOVÆ ET SYNTHÈSES DES ÉLÉMENTS LOURDS

In this talk, I will discuss relations between global parameters of hot and fast-rotating compact stars which do not depend on the equation of state, including a relation connecting the masses of the mass-shedding (Kepler) and static configurations. These relations will then be applied to the GW170817 event by adopting the scenario in which a hypermassive compact star remnant formed in a...

3. The use of non-unified equations of state and its consequence on the modelisation of macroscopic parameters of Neutron Stars

Mlle Lami Suleiman (Laboratoire Univers et Théories)

12/10/2021 13:30

ÉTOILES A NEUTRONS, SUPERNOVÆ ET SYNTHÈSES DES ÉLÉMENTS LOURDS

The observation of macroscopic features can help us investigate matter of Neutron Stars's deepest layers in conditions of density that cannot be reproduced on Earth. The bridge between dense matter physics and Neutron Star observation is provided by the modelisation of macroscopic parameters such as the mass, the radius or the tidal deformability via relativistic equations of hydrodynamics. A...

21. Dense matter equation of state with improved nuclear physics

Dr Guilherme Grams (ip2i)

12/10/2021 13:45

ÉTOILES A NEUTRONS, SUPERNOVÆ ET SYNTHÈSES DES ÉLÉMENTS LOURDS

I will present a new model for dense matter which combines the knowledge of recent theory predictions from chiral EFT, experimental nuclear masses and astrophysical constrains to construct unified equations of state (EoS) describing dense matter in neutron stars (NS), from the crust to the dense core. Based on a recent meta-model for the nuclear component, it allows us to describe the matter...