Outputs (14)

Uncertainties in the production of p nuclides in thermonuclear supernovae determined by Monte Carlo variations (2017)
Journal Article
Nishimura(西村信哉), N., Rauscher, T., Hirschi, R., Murphy, A. S. J., Cescutti, G., & Travaglio, C. (2018). Uncertainties in the production of p nuclides in thermonuclear supernovae determined by Monte Carlo variations. Monthly Notices of the Royal Astronomical Society, 474(3), 3133 -3139. https://doi.org/10.1093/mnras/stx3033

Thermonuclear supernovae originating from the explosion of a white dwarf accreting mass from a companion star have been suggested as a site for the production of p nuclides. Such nuclei are produced during the explosion, in layers enriched with seed... Read More about Uncertainties in the production of p nuclides in thermonuclear supernovae determined by Monte Carlo variations.

Are some CEMP-s stars the daughters of spinstars? (2017)
Journal Article
Choplin, A., Hirschi, R., Meynet, G., & Ekström, S. (2017). Are some CEMP-s stars the daughters of spinstars?. Astronomy and Astrophysics, 607, Article L3. https://doi.org/10.1051/0004-6361/201731948

Carbon-enhanced metal-poor (CEMP)-s stars are long-lived low-mass stars with a very low iron content as well as overabundances of carbon and s-elements. Their peculiar chemical pattern is often explained by pollution from an asymptotic giant branch (... Read More about Are some CEMP-s stars the daughters of spinstars?.

Pre-supernova mixing in CEMP-no source stars (2017)
Journal Article
Choplin, A., Ekström, S., Meynet, G., Maeder, A., Georgy, C., & Hirschi, R. (2017). Pre-supernova mixing in CEMP-no source stars. Astronomy & Astrophysics, 605, A63 -A63. https://doi.org/10.1051/0004-6361/201630182

Context. CEMP-no stars are long-lived low-mass stars with a very low iron content, overabundances of carbon and no or minor signs for the presence of s- or r-elements. Although their origin is still a matter of debate, they are often considered as be... Read More about Pre-supernova mixing in CEMP-no source stars.

Pair-instability Supernova Simulations: Progenitor Evolution, Explosion, and Light Curves (2017)
Journal Article
Hirschi, R. (2017). Pair-instability Supernova Simulations: Progenitor Evolution, Explosion, and Light Curves. Astrophysical Journal, 100 - 100. https://doi.org/10.3847/1538-4357/aa8461

In recent years, the viability of the pair-instability supernova (PISN) scenario for explaining superluminous supernovae has all but disappeared except for a few slowly-evolving examples. However, PISNe are not predicted to be superluminous throughou... Read More about Pair-instability Supernova Simulations: Progenitor Evolution, Explosion, and Light Curves.

Testing a one-dimensional prescription of dynamical shear mixing with a two-dimensional hydrodynamic simulation (2017)
Journal Article
Edelman, P., Röpke, F., Hirschi, R., Georgy, C., & Jones, S. (2017). Testing a one-dimensional prescription of dynamical shear mixing with a two-dimensional hydrodynamic simulation. Astronomy and Astrophysics, 604, Article A25. https://doi.org/10.1051/0004-6361/201629873

Context. The treatment of mixing processes is still one of the major uncertainties in 1D stellar evolution models. This is mostly due to the need to parametrize and approximate aspects of hydrodynamics in hydrostatic codes. In particular, the effect... Read More about Testing a one-dimensional prescription of dynamical shear mixing with a two-dimensional hydrodynamic simulation.

3D hydrodynamic simulations of carbon burning in massive stars (2017)
Journal Article
Cristini, A., Meakin, C., Hirschi, R., Arnett, D., Georgy, C., Viallet, M., & Walkington, I. (2017). 3D hydrodynamic simulations of carbon burning in massive stars. Monthly Notices of the Royal Astronomical Society, 471(1), 279 -300. https://doi.org/10.1093/mnras/stx1535

We present the first detailed 3D hydrodynamic implicit large eddy simulations of turbulent convection of carbon burning in massive stars. Simulations begin with radial profiles mapped from a carbon-burning shell within a 15M circle dot 1D stellar evo... Read More about 3D hydrodynamic simulations of carbon burning in massive stars.

The neutron capture process in the He shell in core-collapse suprenovae: Presolar silicon carbide grains as a diagnostic tool for nuclear astrophysics (2017)
Journal Article
Pignatari, M., Hoppe, P., Trappitsch, R., Fryer, C., Timmes, F., Herwig, F., & Hirschi, R. (2017). The neutron capture process in the He shell in core-collapse suprenovae: Presolar silicon carbide grains as a diagnostic tool for nuclear astrophysics. Geochimica et Cosmochimica Acta, 221, 37-46. https://doi.org/10.1016/j.gca.2017.06.005

Carbon-rich presolar grains are found in primitive meteorites, with isotopic measurements to date suggesting a core-collapse supernovae origin site for some of them. This holds for about 1–2% of presolar silicon carbide (SiC) grains, so-called Type X... Read More about The neutron capture process in the He shell in core-collapse suprenovae: Presolar silicon carbide grains as a diagnostic tool for nuclear astrophysics.

Uncertainties in s-process nucleosynthesis in massive stars determined by Monte Carlo variations (2017)
Journal Article
Nishimura (西村信哉), N., Hirschi, R., Rauscher, T., Murphy, A., & Cescutti, G. (2017). Uncertainties in s-process nucleosynthesis in massive stars determined by Monte Carlo variations. Monthly Notices of the Royal Astronomical Society, 469(2), 1752 -1767. https://doi.org/10.1093/mnras/stx696

The s-process in massive stars produces the weak component of the s-process (nuclei up to A ~ 90), in amounts that match solar abundances. For heavier isotopes, such as barium, production through neutron capture is significantly enhanced in very meta... Read More about Uncertainties in s-process nucleosynthesis in massive stars determined by Monte Carlo variations.

A Chemical Signature from Fast-rotating Low-metallicity Massive Stars: ROA 276 inωCentauri (2017)
Journal Article
Yong, D., Norris, J. E., Da Costa, G. S., Stanford, L. M., Karakas, A. I., Shingles, L. J., …Pignatari, M. (2017). A Chemical Signature from Fast-rotating Low-metallicity Massive Stars: ROA 276 inωCentauri. Astrophysical Journal, 837(2), 176. https://doi.org/10.3847/1538-4357/aa6250

We present a chemical abundance analysis of a metal-poor star, ROA 276, in the stellar system ω Centauri. We confirm that this star has an unusually high [Sr/Ba] abundance ratio. Additionally, ROA 276 exhibits remarkably high abundance ratios, [X/Fe]... Read More about A Chemical Signature from Fast-rotating Low-metallicity Massive Stars: ROA 276 inωCentauri.

Possible pair-instability supernovae at solar metallicity from magnetic stellar progenitors (2017)
Journal Article
Georgy, C., Meynet, G., Ekström, S., Wade, G. A., Petit, V., Keszthelyi, Z., & Hirschi, R. (2017). Possible pair-instability supernovae at solar metallicity from magnetic stellar progenitors. Astronomy & Astrophysics, 599, Article L5. https://doi.org/10.1051/0004-6361/201730401

Near-solar metallicity (and low-redshift) pair-instability supernova (PISN) candidates challenge stellar evolution models. Indeed, at such a metallicity, even an initially very massive star generally loses so much mass by stellar winds that it will a... Read More about Possible pair-instability supernovae at solar metallicity from magnetic stellar progenitors.