129I and 247Cm in Meteorites Constrain the Last Astrophysical Source of Solar r-process Elements. (arXiv:2006.04833v2 [astro-ph.SR] UPDATED)
<a href="http://arxiv.org/find/astro-ph/1/au:+Cote_B/0/1/0/all/0/1">Benoit Côté</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Eichler_M/0/1/0/all/0/1">Marius Eichler</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Yague_A/0/1/0/all/0/1">Andrés Yagüe</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Vassh_N/0/1/0/all/0/1">Nicole Vassh</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Mumpower_M/0/1/0/all/0/1">Matthew R. Mumpower</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Vilagos_B/0/1/0/all/0/1">Blanka Világos</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Soos_B/0/1/0/all/0/1">Benjámin Soós</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Arcones_A/0/1/0/all/0/1">Almudena Arcones</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Sprouse_T/0/1/0/all/0/1">Trevor M. Sprouse</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Surman_R/0/1/0/all/0/1">Rebecca Surman</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Pignatari_M/0/1/0/all/0/1">Marco Pignatari</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Peto_M/0/1/0/all/0/1">Maria K. Pető</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Wehmeyer_B/0/1/0/all/0/1">Benjamin Wehmeyer</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Rauscher_T/0/1/0/all/0/1">Thomas Rauscher</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Lugaro_M/0/1/0/all/0/1">Maria Lugaro</a>
The composition of the early Solar System can be inferred from meteorites.
Many elements heavier than iron were formed by the rapid neutron-capture
process (r process), but the astrophysical sources where this occurred remain
poorly understood. We demonstrate that the near-identical half-lives ($simeq$
15.6 Myr) of the radioactive r-process nuclei 129I and 247Cm preserve their
ratio, irrespective of the time between production and incorporation into the
Solar System. We constrain the last r-process source by comparing the measured
meteoritic 129I / 247Cm = 438 $pm$ 184 to nucleosynthesis calculations based
on neutron star merger and magneto-rotational supernova simulations. Moderately
neutron-rich conditions, often found in merger disk ejecta simulations, are
most consistent with the meteoritic value. Uncertain nuclear physics data limit
our confidence in this conclusion.
The composition of the early Solar System can be inferred from meteorites.
Many elements heavier than iron were formed by the rapid neutron-capture
process (r process), but the astrophysical sources where this occurred remain
poorly understood. We demonstrate that the near-identical half-lives ($simeq$
15.6 Myr) of the radioactive r-process nuclei 129I and 247Cm preserve their
ratio, irrespective of the time between production and incorporation into the
Solar System. We constrain the last r-process source by comparing the measured
meteoritic 129I / 247Cm = 438 $pm$ 184 to nucleosynthesis calculations based
on neutron star merger and magneto-rotational supernova simulations. Moderately
neutron-rich conditions, often found in merger disk ejecta simulations, are
most consistent with the meteoritic value. Uncertain nuclear physics data limit
our confidence in this conclusion.
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