stars; nucleosynthesis; stellar evolution; nucleosynthesis; stars; stellar evolution
Liu N., Savina M., Davis A., Gallino R., Straniero O., Gyngard F., Pellin M., Willingham M., Dauphas N., Pignatari M. (2014), Barium Isotopic Composition of Mainstream Silicon Carbides from Murchison: Constraints for s-process Nucleosynthesis in Asymptotic Giant Branch Stars, in The Astrophysical Journal
, 786(1), 66.
Fujiya W., Hoppe P., Zinner E., Pignatari M., Herwig F. (2014), A Born-Again AGB Star Origin of Type AB Silicon Carbide Grains Inferred from Radiogenic Sulfur-32, in 45th Lunar and Planetary Science Conference
, 1777, 1515.
Yong D., Alves Brito A., Da Costa G., Alonso Garcia J., Karakas A., Pignatari M., et al.... (2014), Chemical abundances in bright giants of the globular cluster M62 (NGC 6266), in Monthly Notices of the Royal Astronomical Society
, 439(3), 2638.
Praena J., Pignatari M., et al. (2014), Current quests in nucleosynthesis: present and future neutron-induced reaction measurements, in EPJ Web of Conferences
, 66, 66.
Zureg P., et al.... (2014), Experimental neutron capture data of 58Ni from the CERN n_TOF facility, in Physical Review C
, 89(2), 014605.
Nishimura N., Hirschi R., Pignatari M., et al. (2014), Impact of the uncertainty in alpha-captures on 22Ne on the weak s-process in massive stars, in AIP Conference Proceedings
Denissenkov P., Truran J., Pignatari M., et al. (2014), MESA and NuGrid simulations of classical novae: CO and ONe nova nucleosynthesis, in Monthly Notices of the Royal Astronomical Society
, 442(3), 2058.
Lederer C., et al... (2014), Ni62(n,gamma) and Ni63(n,gamma) cross sections measured at the n_TOF facility at CERN, in Physical Review C
, 89(2), 025810.
Fujiya Wataru, Hoppe P., Zinner E., Pignatari M., Herwig F. (2013), Evidence for Radiogenic Sulfur-32 in Type AB Presolar Silicon Carbide Grains?, in ApJ Letters
, 776(2), 6.
Jadhav M., Pignatari M., Herwig F., Zinner E., Gallino R., Huss G. (2013), Relics of Ancient Post-AGB Stars in a Primitive Meteorite, in ApJ Letters
, 777(2), 7.
Barbuy B., Chiappini C., Cantelli E., Depagne E., Pignatari M., et al., High-resolution abundance analysis of red giants in the globular cluster NGC 6522, in Astronomy & Astrophysics
In the Solar System only less than 2% of the nuclear species are heavier than H and He. Those abundances are the result of the chemical enrichment of the Galaxy from many generations of stars. Besides the solar abundance distribution, information about stellar evolution and nucleosynthesis are obtained from stellar spectroscopic observations of different types of stars, in our Galaxy or more far away in extragalactic systems. Complementary information is hidden in tiny dust of presolar origin found in primitive meteorites (e.g., nano-diamonds, silicon carbides, graphites). Such grains were produced in stars before the formation of the Solar System, and were trapped into meteorites during their formation. They carry the isotopic signature of the nucleosynthesis processes in their respective parent star, and enable detailed laboratory abundance determinations. The stars that made this dust cannot be seen anymore, but it is still possible to "touch" them. In the cross disciplinary context of nuclear astrophysics, this project aims to shade new light into many open questions, addressing in first instance the fundamental question of how elements form in our galaxy and in the universe. The direction of research is twofold. First, a new interpretation of the abundances measured in presolar dust from massive stars is provided. We demonstrate that they are not made from extensive mixing of different layers of supernovae as it was assumed until now, but instead they only condensed from the external carbon-rich stellar layers of the supernova explosion. Thanks to this project, presolar grains can be correctly used as a constraint on massive star supernovae. Second, also thanks to the AMBIZIONE support since 2010, we made a fundamental advance in the knowledge of mixing properties of low-mass and intermediate-mass stars in their later evolutionary stages, studying the impact of Kelvin-Helmholtz instabilities and gravity waves on their evolution and on the production of the elements.