Can neutron-star mergers explain r-process elements in the oldest stars?
In plain words
Some very old stars already contain r-process elements, yet merging neutron stars need time to spiral together.
Precise statement
Determine whether merger delay-time distributions (minimum ~10 Myr, $\mathrm{d}N/\mathrm{d}t \sim t^{-1}$) with natal kicks and inhomogeneous mixing reproduce r-process enrichment in ultra-faint dwarf galaxies such as Reticulum II and the decline of $[\mathrm{Eu}/\mathrm{Fe}]$ at $[\mathrm{Fe}/\mathrm{H}] > -1$ in the Galactic disk, or whether a prompt source is required. Answer: yes or no from galactic chemical evolution models.
What would settle it
Chemical-evolution models with measured delay times and kicks fit to large samples of Eu abundances in dwarf galaxies and the disk, with and without a prompt source.
Parent problems
- Special case of Which site dominates the r-process inventory of the Milky Way? · open · from revision 1
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