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Retainment of r-process material in dwarf galaxies
Beniamini, Paz; Dvorkin, Irina; Silk, Joe
AA(Department of Physics, The George Washington University, Washington, DC 20052, USA; Astronomy, Physics and Statistics Institute of Sciences (APSIS) 0000-0001-7833-1043), AB(Max Planck Institute for Gravitational Physics (Albert Einstein Institute), Am Mühlenberg 1, Potsdam-Golm, 14476, Germany; Institut d'Astrophysique de Paris UMR 7095 Université Pierre et Marie Curie-Paris 06; CNRS 98 bis bd Arago, 75014 Paris, France), AC(Institut d'Astrophysique de Paris UMR 7095 Université Pierre et Marie Curie-Paris 06; CNRS 98 bis bd Arago, 75014 Paris, France; Department of Physics and Astronomy, The Johns Hopkins University, Baltimore MD21218 USA)
Monthly Notices of the Royal Astronomical Society, Advance Access (MNRAS Homepage)
Publication Date:
Astronomy Keywords:
galaxies: dwarf, stars: neutron, stars: abundances;
Abstract Copyright:
2018 The Author(s) Published by Oxford University Press on behalf of the Royal Astronomical Society
Bibliographic Code:


The synthesis of r-process elements is known to involve extremely energetic explosions. At the same time, recent observations find significant r-process enrichment even in extremely small ultra-faint dwarf (UFD) galaxies. This raises the question of retainment of those elements within their hosts. We estimate the retainment fraction and find that it is large ˜0.9, unless the r-process event is very energetic (≳ 1052erg) and / or the host has lost a large fraction of its gas prior to the event. We estimate the r-process mass per event and rate as implied by abundances in UFDs, taking into account imperfect retainment and different models of UFD evolution. The results are consistent with previous estimates (Beniamini et al. 2016b) and with the constraints from the recently detected macronova accompanying a neutron star merger (GW170817). We also estimate the distribution of abundances predicted by these models. We find that ˜0.07 of UFDs should have r-process enrichment. The results are consistent with both the mean values and the fluctuations of [Eu/Fe] in galactic metal poor stars, supporting the possibility that UFDs are the main 'building blocks' of the galactic halo population.
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