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Outputs (104)

NuGrid Stellar Data Set. II. Stellar Yields from H to Bi for Stellar Models with MZAMS = 1 to 25 M? and Z = 0.0001 to 0.02 (2018)
Journal Article
Ritter, C., Herwig, F., Jones, S., Pignatari, M., Fryer, C., & Hirschi, R. (2018). NuGrid Stellar Data Set. II. Stellar Yields from H to Bi for Stellar Models with MZAMS = 1 to 25 M? and Z = 0.0001 to 0.02. Monthly Notices of the Royal Astronomical Society, 480(1), 538-571. https://doi.org/10.1093/mnras/sty1729

We provide here a significant extension of the NuGrid Set 1 models in mass coverage and toward lower metallicity, adopting the same physics assumptions. The combined data set now includes the initial masses MZAMS/?M? = 1, 1.65, 2, 3, 4, 5, 6, 7, 12,... Read More about NuGrid Stellar Data Set. II. Stellar Yields from H to Bi for Stellar Models with MZAMS = 1 to 25 M? and Z = 0.0001 to 0.02.

OGLE14-073 – a promising pair-instability supernova candidate (2018)
Journal Article
Kozyreva, A., Kromer, M., Noebauer, U. M., & Hirschi, R. (2018). OGLE14-073 – a promising pair-instability supernova candidate. Monthly Notices of the Royal Astronomical Society, 479(3), 3106 - 3114. https://doi.org/10.1093/mnras/sty983

The recently discovered bright Type? II supernova OGLE14-073 evolved very slowly. The light curve rose to maximum for 90?d from discovery and then declined at a rate compatible with the radioactive decay of 56Co. In this study, we show that a pair-in... Read More about OGLE14-073 – a promising pair-instability supernova candidate.

Uncertainties in s -process nucleosynthesis in low mass stars determined from Monte Carlo variations (2018)
Journal Article
Cescutti, G., Hirschi, R., Nishimura, N., den Hartogh, J. W., Rauscher, T., Murphy, A. S. J., & Cristallo, S. (2018). Uncertainties in s -process nucleosynthesis in low mass stars determined from Monte Carlo variations. Monthly Notices of the Royal Astronomical Society, 478(3), 4101-4127. https://doi.org/10.1093/mnras/sty1185

The main s-process taking place in low mass stars produces about half of the elements heavier than iron. It is therefore very important to determine the importance and impact of nuclear physics uncertainties on this process. We have performed extensi... Read More about Uncertainties in s -process nucleosynthesis in low mass stars determined from Monte Carlo variations.

Abundance uncertainties obtained with the PIZBUIN framework for Monte Carlo reaction rate variations (2018)
Journal Article
Rauscher, T., Nishimura, N., Cescutti, G., Hirschi, R., & Murphy, A. S. J. (2018). Abundance uncertainties obtained with the PIZBUIN framework for Monte Carlo reaction rate variations. AIP conference proceedings, 1947(1), https://doi.org/10.1063/1.5030819

Uncertainties in nucleosynthesis models originating from uncertainties in astrophysical reaction rates were estimated in a Monte Carlo variation procedure. Thousands of rates were simultaneously varied within individual, temperature-dependent errors... Read More about Abundance uncertainties obtained with the PIZBUIN framework for Monte Carlo reaction rate variations.

Sensitivity to neutron captures and ß -decays of the enhanced s-process in rotating massive stars at low metallicities (2018)
Journal Article
Hirschi. (2018). Sensitivity to neutron captures and ß -decays of the enhanced s-process in rotating massive stars at low metallicities. Journal of Physics: Conference Series, 12051. https://doi.org/10.1088/1742-6596/940/1/012051

The s-process in massive stars, producing nuclei up to A ˜ 90, has a different behaviour at low metallicity if stellar rotation is significant. This enhanced s-process is distinct from the s-process in massive stars around solar metallicity, and deta... Read More about Sensitivity to neutron captures and ß -decays of the enhanced s-process in rotating massive stars at low metallicities.

Nucleosynthesis in the first massive stars (2018)
Journal Article
Hirschi. (2018). Nucleosynthesis in the first massive stars. Journal of Physics: Conference Series, 012021 -?. https://doi.org/10.1088/1742-6596/940/1/012021

The nucleosynthesis in the first massive stars may be constrained by observing the surface composition of long-lived very iron-poor stars born around 10 billion years ago from material enriched by their ejecta. Many interesting clues on physical proc... Read More about Nucleosynthesis in the first massive stars.

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.