Raphaël Hirschi
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View article: 3D synthetic convective velocity fields to initialize core-collapse supernova simulations from 1D progenitors
3D synthetic convective velocity fields to initialize core-collapse supernova simulations from 1D progenitors Open
Core-collapse supernovae (CCSNe) are among the most energetic and complex astrophysical phenomena, requiring three-dimensional (3D) simulations to capture their intricate explosion mechanisms. One of the key ingredients for such simulation…
View article: Trans-Fe elements from type Ia supernovae
Trans-Fe elements from type Ia supernovae Open
Context. A type Ia supernova (SNIa) marks the catastrophic explosion of a white dwarf in a binary system. These events play a crucial role in galactic chemical evolution and serve as pivotal standardisable candles for measuring cosmic dist…
View article: The fate of rotating massive stars across cosmic times
The fate of rotating massive stars across cosmic times Open
The initial mass and metallicity of stars both have a strong impact on their fate. Stellar axial rotation also has a strong impact on the structure and evolution of massive stars. In this study, we exploit the large grid of GENEC models, c…
View article: The impact of wind mass loss on nucleosynthesis and yields of very massive stars at low metallicity
The impact of wind mass loss on nucleosynthesis and yields of very massive stars at low metallicity Open
The chemical feedback from stellar winds in low metallicity ( Z ) environments is key to understanding the evolution of globular clusters and the early Universe. With a disproportionate amount of mass lost from the most massive stars ( M >…
View article: Stellar Evolution and Convection in 3D Hydrodynamic Simulations of a Complete Burning Phase
Stellar Evolution and Convection in 3D Hydrodynamic Simulations of a Complete Burning Phase Open
Our understanding of stellar evolution and nucleosynthesis is limited by the uncertainties coming from the complex multi-dimensional processes in stellar interiors, such as convection and nuclear burning. Three-dimensional stellar models c…
View article: Evolving massive stars to core collapse with GENEC: Extension of equation of state, opacities and effective nuclear network
Evolving massive stars to core collapse with GENEC: Extension of equation of state, opacities and effective nuclear network Open
Context. Stars with initial mass above roughly 8 M ⊙ will evolve to form a core made of iron group elements, at which point no further exothermic nuclear reactions between charged nuclei may prevent the core collapse. Electron capture, neu…
View article: New Wolf–Rayet wind yields and nucleosynthesis of Helium stars
New Wolf–Rayet wind yields and nucleosynthesis of Helium stars Open
Strong metallicity-dependent winds dominate the evolution of core He-burning, classical Wolf–Rayet (cWR) stars, which eject both H and He-fusion products such as $^{14}$N, $^{12}$C, $^{16}$O, $^{19}$F, $^{22}$Ne, and $^{23}$Na during their…
View article: Evolving massive stars to core collapse with GENEC: Extension of equation of state, opacities and effective nuclear network
Evolving massive stars to core collapse with GENEC: Extension of equation of state, opacities and effective nuclear network Open
Stars with initial mass above roughly 8 solar masses will evolve to form a core made of iron group elements at which point no further exothermic nuclear reactions between charged nuclei may prevent the core collapse. Electron captures, neu…
View article: Grids of stellar models with rotation
Grids of stellar models with rotation Open
Context. Grids of stellar evolution models with rotation using the Geneva stellar evolution code (G ENEC ) have been published for a wide range of metallicities. Aims. We introduce the last remaining grid of G ENEC models, with a metallici…
View article: Shell mergers in the late stages of massive star evolution: new insight from 3D hydrodynamic simulations
Shell mergers in the late stages of massive star evolution: new insight from 3D hydrodynamic simulations Open
One-dimensional (1D) stellar evolution models are widely used across various astrophysical fields, however they are still dominated by important uncertainties that deeply affect their predictive power. Among those, the merging of independe…
View article: Shell mergers in the late stages of massive star evolution: new insight from 3D hydrodynamic simulations
Shell mergers in the late stages of massive star evolution: new insight from 3D hydrodynamic simulations Open
One-dimensional (1D) stellar evolution models are widely used across various astrophysical fields, however they are still dominated by important uncertainties that deeply affect their predictive power. Among those, the merging of independe…
View article: New Wolf-Rayet wind yields and nucleosynthesis of Helium stars
New Wolf-Rayet wind yields and nucleosynthesis of Helium stars Open
Strong metallicity-dependent winds dominate the evolution of core He-burning, classical Wolf-Rayet (cWR) stars, which eject both H and He-fusion products such as 14N, 12C, 16O, 19F, 22Ne and 23Na during their evolution. The chemical enrich…
View article: Grids of stellar models with rotation VIII: Models from 1.7 to 500 $M_\odot$ at metallicity $Z = 10^{-5}$
Grids of stellar models with rotation VIII: Models from 1.7 to 500 $M_\odot$ at metallicity $Z = 10^{-5}$ Open
Grids of stellar evolution models with rotation using the Geneva stellar evolution code (Genec) have been published for a wide range of metallicities. We introduce the last remaining grid of Genec models, with a metallicity of $Z=10^{-5}$.…
View article: 3D simulations of a neon burning convective shell in a massive star
3D simulations of a neon burning convective shell in a massive star Open
The treatment of convection remains a major weakness in the modelling of stellar evolution with one-dimensional (1D) codes. The ever-increasing computing power makes now possible to simulate in three-dimensional (3D) part of a star for a f…
View article: 3D simulations of convective shell Neon-burning in a massive star
3D simulations of convective shell Neon-burning in a massive star Open
The treatment of convection remains a major weakness in the modelling of stellar evolution with one-dimensional (1D) codes. The ever increasing computing power makes now possible to simulate in 3D part of a star for a fraction of its life,…
View article: Rapidly rotating Population III stellar models as a source of primary nitrogen
Rapidly rotating Population III stellar models as a source of primary nitrogen Open
Context. The first stars might have been fast rotators. This would have important consequences for their radiative, mechanical, and chemical feedback. Aims. We discuss the impact of fast initial rotation on the evolution of massive Populat…
View article: Rapidly rotating Population III stellar models as a source of primary nitrogen
Rapidly rotating Population III stellar models as a source of primary nitrogen Open
The first stars might have been fast rotators. This would have important consequences for their radiative, mechanical and chemical feedback. We discuss the impact of fast initial rotation on the evolution of massive Population III models a…
View article: Very massive star models
Very massive star models Open
Context. In addition to being spectacular objects, very massive stars (VMSs) are suspected to have a tremendous impact on their environment and on cosmic evolution in general. The nucleosynthesis both during their advanced stages and their…
View article: The Nuclear Reaction Network WinNet
The Nuclear Reaction Network WinNet Open
We present the state-of-the-art single-zone nuclear reaction network WinNet , which is capable of calculating the nucleosynthetic yields of a large variety of astrophysical environments and conditions. This ranges from the calculation of t…
View article: Very Massive Star Models: I. Impact of Rotation and Metallicity and Comparisons with Observations
Very Massive Star Models: I. Impact of Rotation and Metallicity and Comparisons with Observations Open
In addition to being spectacular objects, Very Massive Stars (VMS) are suspected to have a tremendous impact on their environment and on the whole cosmic evolution. The nucleosynthesis both during their advanced stages and their final expl…
View article: Stellar Wind Yields of Very Massive Stars
Stellar Wind Yields of Very Massive Stars Open
The most massive stars provide an essential source of recycled material for young clusters and galaxies. While very massive stars (VMS, M>100M) are relatively rare compared to O stars, they lose disproportionately large amounts of mass alr…
View article: 3D stellar evolution: hydrodynamic simulations of a complete burning phase in a massive star
3D stellar evolution: hydrodynamic simulations of a complete burning phase in a massive star Open
Our knowledge of stellar evolution is driven by one-dimensional (1D) simulations. 1D models, however, are severely limited by uncertainties on the exact behaviour of many multidimensional phenomena occurring inside stars, affecting their s…
View article: 3D stellar evolution: hydrodynamic simulations of a complete burning phase in a massive star
3D stellar evolution: hydrodynamic simulations of a complete burning phase in a massive star Open
Our knowledge of stellar evolution is driven by one-dimensional (1D) simulations. 1D models, however, are severely limited by uncertainties on the exact behaviour of many multi-dimensional phenomena occurring inside stars, affecting their …
View article: The nuclear reaction network WinNet
The nuclear reaction network WinNet Open
We present the state-of-the-art single-zone nuclear reaction network WinNet that is capable of calculating the nucleosynthetic yields of a large variety of astrophysical environments and conditions. This ranges from the calculation of the …
View article: Turbulence and nuclear reactions in 3D hydrodynamics simulations of massive stars
Turbulence and nuclear reactions in 3D hydrodynamics simulations of massive stars Open
Our knowledge of massive star evolution and nucleosynthesis is limited by uncertainties related to multi-dimensional processes taking place in stellar interiors. Recently, theoretical works have started to improve 1D stellar evolution code…
View article: Spin-down and reduced mass loss in early-type stars with large-scale magnetic fields
Spin-down and reduced mass loss in early-type stars with large-scale magnetic fields Open
Magnetism can greatly impact the evolution of stars. In some stars with OBA spectral types there is direct evidence via the Zeeman effect for stable, large-scale magnetospheres, which lead to the spin-down of the stellar surface and reduce…
View article: The effects of surface fossil magnetic fields on massive star evolution: IV. Grids of models at Solar, LMC, and SMC metallicities
The effects of surface fossil magnetic fields on massive star evolution: IV. Grids of models at Solar, LMC, and SMC metallicities Open
Magnetic fields can drastically change predictions of evolutionary models of massive stars via mass-loss quenching, magnetic braking, and efficient angular momentum transport, which we aim to quantify in this work. We use the mesa software…
View article: The effects of surface fossil magnetic fields on massive star evolution: IV. Grids of models at Solar, LMC, and SMC metallicities
The effects of surface fossil magnetic fields on massive star evolution: IV. Grids of models at Solar, LMC, and SMC metallicities Open
Magnetic fields can drastically change predictions of evolutionary models of massive stars via mass-loss quenching, magnetic braking, and efficient angular momentum transport, which we aim to quantify in this work. We use the MESA software…
View article: Realistic 3D hydrodynamics simulations find significant turbulent entrainment in massive stars
Realistic 3D hydrodynamics simulations find significant turbulent entrainment in massive stars Open
Our understanding of stellar structure and evolution coming from one-dimensional (1D) stellar models is limited by uncertainties related to multidimensional processes taking place in stellar interiors. 1D models, however, can now be tested…
View article: Very massive star winds as sources of the short-lived radioactive isotope <sup>26</sup>Al
Very massive star winds as sources of the short-lived radioactive isotope <sup>26</sup>Al Open
Context. The 26 Al short-lived radioactive nuclide is the source of the observed galactic diffuse γ -ray emission at 1.8 MeV. While different sources of 26 Al have been explored, such as asymptotic giant branch stars, massive stellar winds…