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Search for Na in novae supported by a novel method for measuring femtosecond nuclear lifetimes.
Nat Commun
September 2023
Irfu, CEA, Université Paris-Saclay, Gif-sur-Yvette, France.
Classical novae are thermonuclear explosions in stellar binary systems, and important sources of Al and Na. While γ rays from the decay of the former radioisotope have been observed throughout the Galaxy, Na remains untraceable. Its half-life (2.
View Article and Find Full Text PDFNew implications for the origin of the IAB main group iron meteorites and the isotopic evolution of the noncarbonaceous (NC) reservoir.
Earth Planet Sci Lett
June 2020
Department of Geology, University of Maryland, College Park, Maryland, 20742, USA.
The origin of the IAB main group (MG) iron meteorites is explored through consideration of W isotopic compositions, thermal modeling of Al decay, and mass independent (nucleosynthetic) Mo isotopic compositions of planetesimals formed in the noncarbonaceous (NC) protosolar isotopic reservoir. A refined W model age for the meteorites Campo del Cielo, Canyon Diablo, and Nantan suggests that the IAB-MG parent body underwent some form of metal-silicate segregation as early as 5.3 ± 0.
View Article and Find Full Text PDFInverse Kinematic Study of the (26g)Al(d,p)(27)Al Reaction and Implications for Destruction of (26)Al in Wolf-Rayet and Asymptotic Giant Branch Stars.
Phys Rev Lett
August 2015
Department of Physics, University of Surrey, Guildford GU2 7XH, United Kingdom.
In Wolf-Rayet and asymptotic giant branch (AGB) stars, the (26g)Al(p,γ)(27)Si reaction is expected to govern the destruction of the cosmic γ-ray emitting nucleus (26)Al. The rate of this reaction, however, is highly uncertain due to the unknown properties of key resonances in the temperature regime of hydrogen burning. We present a high-resolution inverse kinematic study of the (26g)Al(d,p)(27)Al reaction as a method for constraining the strengths of key astrophysical resonances in the (26g)Al(p,γ)(27)Si reaction.
View Article and Find Full Text PDFHf-W-Th evidence for rapid growth of Mars and its status as a planetary embryo.
Nature
May 2011
Origins Laboratory, Department of the Geophysical Sciences and Enrico Fermi Institute, The University of Chicago, 5734 South Ellis Avenue, Chicago, Illinois 60637, USA.
Terrestrial planets are thought to have formed through collisions between large planetary embryos of diameter ∼1,000-5,000 km. For Earth, the last of these collisions involved an impact by a Mars-size embryo that formed the Moon 50-150 million years (Myr) after the birth of the Solar System. Although model simulations of the growth of terrestrial planets can reproduce the mass and dynamical parameters of the Earth and Venus, they fall short of explaining the small size of Mars.
View Article and Find Full Text PDFEvidence for a late supernova injection of 60Fe into the protoplanetary disk.
Science
May 2007
Geological Institute, University of Copenhagen, Øster Voldgade 10, DK-1350, Denmark.
High-precision 60Fe-60Ni isotope data show that most meteorites originating from differentiated planetesimals that accreted within 1 million years of the solar system's formation have 60Ni/58Ni ratios that are approximately 25 parts per million lower than samples from Earth, Mars, and chondrite parent bodies. This difference indicates that the oldest solar system planetesimals formed in the absence of 60Fe. Evidence for live 60Fe in younger objects suggests that 60Fe was injected into the protoplanetary disk approximately 1 million years after solar system formation, when 26Al was already homogeneously distributed.
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