Zobrazeno 1 - 10
of 219
pro vyhledávání: '"Ekström Sylvia"'
Autor:
Griffiths, Adam, Aloy, Miguel-Á, Hirschi, Raphael, Reichert, Moritz, Obergaulinger, Martin, Whitehead, Emily E., Martinet, Sébastien, Ekström, Sylvia, Meynet, Georges
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, neutrino losse
Externí odkaz:
http://arxiv.org/abs/2408.03368
Autor:
Sibony, Yves, Shepherd, Kendall G., Yusof, Norhasliza, Hirschi, Raphael, Chambers, Caitlan, Tsiatsiou, Sophie, Nandal, Devesh, Sciarini, Luca, Moyano, Facundo D., Bétrisey, Jérôme, Buldgen, Gaël, Georgy, Cyril, Ekström, Sylvia, Eggenberger, Patrick, Meynet, Georges
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 $Z=10^{-5}$. We study t
Externí odkaz:
http://arxiv.org/abs/2407.06739
Autor:
Nandal, Devesh, Zwick, Lorenz, Whalen, Daniel J., Mayer, Lucio, Ekström, Sylvia, Meynet, Georges
Publikováno v:
A&A 689, A351 (2024)
The first stars formed over five orders of magnitude in mass by accretion in primordial dark matter halos. We study the evolution of massive, very massive and supermassive primordial (Pop III) stars over nine orders of magnitude in accretion rate. We
Externí odkaz:
http://arxiv.org/abs/2407.06994
Publikováno v:
A&A 689, A169 (2024)
Accreting supermassive stars of $\gtrsim 10^{5}\,M_\odot$ will eventually collapse directly to a black hole via the general relativistic (GR) instability. Such direct collapses of supermassive stars are thought to be a possible formation channel for
Externí odkaz:
http://arxiv.org/abs/2406.18040
Publikováno v:
A&A 688, A71 (2024)
Stellar winds are one of the most important drivers of massive star evolution and a vital source of chemical, mechanical, and radiative feedback. Despite its significance, mass loss remains a major uncertainty in stellar evolution models. Particularl
Externí odkaz:
http://arxiv.org/abs/2404.14488
Autor:
Gormaz-Matamala, Alex Camilo, Cuadra, Jorge, Ekström, Sylvia, Meynet, Georges, Curé, Michel, Belczynski, Krzysztof
Publikováno v:
A&A 687, A290 (2024)
We use Geneva-evolution-code to run evolutionary tracks for stellar masses ranging from $20$ to $85$ $M_\odot$ at SMC metallicity ($Z=0.002$). We upgrade the recipe for stellar winds by adopting our self-consistent m-CAK prescription, which reduces t
Externí odkaz:
http://arxiv.org/abs/2404.07570
Autor:
Nandal, Devesh, Regan, John A., Woods, Tyrone E., Farrell, Eoin, Ekström, Sylvia, Meynet, Georges
The chemical enrichment of the early Universe is a crucial element in the formation and evolution of galaxies, and Population III (PopIII) stars must play a vital role in this process. In this study, we examine metal enrichment from massive stars in
Externí odkaz:
http://arxiv.org/abs/2402.03428
Autor:
Nandal, Devesh, Meynet, Georges, Ekström, Sylvia, Moyano, Facundo D., Eggenberger, Patrick, Choplin, Arthur, Georgy, Cyril, Farrell, Eoin, Maeder, Andre
The physics of stellar rotation plays a crucial role in the evolution of stars, their final fate and the properties of compact remnants. Diverse approaches have been adopted to incorporate the effects of rotation in stellar evolution models. This stu
Externí odkaz:
http://arxiv.org/abs/2312.13340
Autor:
Sciarini, Luca, Ekström, Sylvia, Eggenberger, Patrick, Meynet, Georges, Fragos, Tassos, Song, Han Feng
Binary evolution codes are essential tools to help in understanding the evolution of binary systems. They contain a great deal of physics, for example stellar evolution, stellar interactions, mass transfer, tides, orbital evolution. Since many of the
Externí odkaz:
http://arxiv.org/abs/2312.08437
Publikováno v:
A&A 680, A101 (2023)
We study the differences between models computed with Ledoux and Schwarzschild criteria on the internal structure, evolutionary track in the Hertzsprung-Russell diagram (HRD), lifetimes, evolution of the surface abundances and velocities, and masses
Externí odkaz:
http://arxiv.org/abs/2310.18139