255 citations · 5.8k across the 143 of their papers we have counts for
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Nuclear Physics Mid Term Plan at LNGS
R. Buompane, F. Cavanna, C. Curceanu +59
The Istituto Nazionale di Fisica Nucleare-Laboratori Nazionali del Gran Sasso (LNGS) is one of the largest underground physics laboratory, a very peculiar environment suited for ex…
The s Process and Beyond
Maria Lugaro, Marco Pignatari, René Reifarth +1
Neutron captures produce the vast majority of abundances of elements heavier than iron in the Universe. Beyond the classical slow (s) and rapid (r) processes, there is observationa…
Improved thermonuclear rate of Ti(,)V and its astrophysical implication in rp-process
S. Q. Hou, C. Iliadis, M. Pignatari +4
Accurate Ti(,)V reaction rates are crucial for understanding the nucleosynthesis path of the rapid capture process (rp-process) that occurs in X-ray bursts. We…
The s process in massive stars, a benchmark for neutron capture reaction rates
Marco Pignatari, Roberto Gallino, Rene Reifarth
A clear definition of the contribution from the slow neutron-capture process (s process) to the solar abundances between Fe and the Sr-Zr region is a crucial challenge for nuclear…
Production of radioactive Na in core-collapse supernovae: the Ne-E(L) component in presolar grains and its possible consequences on supernova observations
M. Pignatari, S. Amari, P. Hoppe +8
Presolar graphite grains carry the isotopic signatures of their parent stars. A significant fraction of presolar graphites shows isotopic abundance anomalies relative to solar for…
SHADES -- Ne(,n)Mg reaction rate in the Gamow window
David Rapagnani, Chemseddine Ananna, Antonino Di Leva +4
Neutron capture reactions are the main contributors to the synthesis of the heavy elements through the s-process. Together with C(,n)16O, which has recently been measured…
Galactic chemical evolution of short-lived radioactive isotopes produced by explosive nucleosynthesis: Fe and Mn
Thomas C. L. Truemam, Andrés Yagüe López, Maria Lugaro +1
Several short-lived radionuclides (SLRs) are know to have existed in the early Solar System (ESS). These species, which typically decay with half-lives of the order of a few millio…
Impact of the latest 22Ne+α reaction rates on nucleosynthesis in massive stars and galactic chemical evolution
Emma Kotar, Shuya Ota, Allyson Dewey +3
In massive stars (initial mass of > 9 solar masses), the weak s (slow neutron capture) process produces elements between Fe and Zr, enriching the Galaxy with these elements through…
3D Macro Physics and Light Odd-Z Element Production in O-C Shell Mergers: Implications for production and radiogenic heating inventories of rocky exoplanets
Joshua Issa, Falk Herwig, Stephen J. Mojzsis +1
The light odd-Z elements P, Cl, K, and Sc are underproduced in galactic chemical evolution models compared to spectroscopic observations of stars in the Milky Way. The most promisi…
The SPAr burning: proton captures powering carbon-oxygen shell mergers in massive stars
L. Roberti, M. Pignatari
Carbon-oxygen (C-O) shell mergers in massive stars play a crucial role in both nucleosynthesis and the final stages of stellar evolution. These convective-reactive events significa…
Impact of 3D macro physics and nuclear physics on the p nuclei in O-C shell mergers
Joshua Issa, Falk Herwig, Pavel Denissenkov +1
O-C shell mergers in massive stars are a site for producing the p nuclei by the process, but 1D stellar models rely on mixing length theory, which does not match the radial vel…
Reconstructing the Milky Way chemical map with Galactic Chemical Evolution tool OMEGA+ from SDSS-MWM
Viola Hegedűs, Szabolcs Mészáros, Blanka Világos +4
We obtain two-infall galactic chemical evolution (GCE) models simulating the chemical evolution of the Milky Way as constrained by a golden sample of stellar abundances o…
The Occurrence and Impact of Carbon-Oxygen Shell Mergers in Massive Stars
L. Roberti, M. Pignatari, H. E. Brinkman +6
In their final stages before undergoing a core-collapse supernova, massive stars may experience mergers between internal shells where carbon (C) and oxygen (O) are consumed as fuel…