Using stellar observations to trace the formation processes of Mo, Ru, Pd, and Ag

TY - GEN

T1 - Using stellar observations to trace the formation processes of Mo, Ru, Pd, and Ag

AU - Hansen, Camilla J.

AU - Hansen, Terese T.

AU - Arcones, Almudena

AU - Andersen, Anja C.

PY - 2018

Y1 - 2018

N2 - The exact formation mechanism of many heavy elements remains unknown. Models of the formation site and environment have greatly improved over the past decades, and experiments have provided new data for many of the heavy isotopes. However, much information is still missing to fully describe the neutron-capture formation processes and their sites. Stellar observations combined with mass spectroscopy of meteorites can help to place some of the needed constraints. This, in turn, will help to improve the models and our knowledge on the formation channels creating these heavy elements. Recent studies of Mo, Ru, Pd, and Ag showed that different processes or environments other than the main r-process (forming, e.g., Eu) are needed to explain the production (and observations) of elements with 40 < Z < 50. An observational study of Mo-Ag is presented, where stellar abundances are compared to meteoritic isotopic abundances (at metallicities [Fe/H] > -1.5) to extract information on differences or similarities in their production. Finally, the number of formation processes needed to describe the chemical composition in low metallicity stars ([Fe/H] < -2.5) is discussed.

AB - The exact formation mechanism of many heavy elements remains unknown. Models of the formation site and environment have greatly improved over the past decades, and experiments have provided new data for many of the heavy isotopes. However, much information is still missing to fully describe the neutron-capture formation processes and their sites. Stellar observations combined with mass spectroscopy of meteorites can help to place some of the needed constraints. This, in turn, will help to improve the models and our knowledge on the formation channels creating these heavy elements. Recent studies of Mo, Ru, Pd, and Ag showed that different processes or environments other than the main r-process (forming, e.g., Eu) are needed to explain the production (and observations) of elements with 40 < Z < 50. An observational study of Mo-Ag is presented, where stellar abundances are compared to meteoritic isotopic abundances (at metallicities [Fe/H] > -1.5) to extract information on differences or similarities in their production. Finally, the number of formation processes needed to describe the chemical composition in low metallicity stars ([Fe/H] < -2.5) is discussed.

U2 - 10.1088/1742-6596/940/1/012009

DO - 10.1088/1742-6596/940/1/012009

M3 - Conference article

AN - SCOPUS:85042438639

SN - 1742-6588

VL - 940

JO - Journal of Physics: Conference Series

JF - Journal of Physics: Conference Series

IS - 1

M1 - 012009

T2 - 7th Nuclear Physics in Astrophysics Conference, NPA 2015

Y2 - 18 May 2015 through 22 May 2015

ER -