paper

The lanthanide fraction distribution in metal-poor stars: a test of neutron star mergers as the dominant r-process site

arXiv:1905.01814 · doi:10.3847/1538-4357/ab3291

Abstract

Multimessenger observations of the neutron star merger GW170817 and its kilonova proved that neutron star mergers can synthesize large quantities of r-process elements. If neutron star mergers in fact dominate all r-process element production, then the distribution of kilonova ejecta compositions should match the distribution of r-process abundance patterns observed in stars. The lanthanide fraction (XLa) is a measurable quantity in both kilonovae and metal-poor stars, but it has not previously been explicitly calculated for stars. Here, we compute the lanthanide fraction distribution of metal-poor stars ([Fe/H] < -2.5) to enable comparison to current and future kilonovae. The full distribution peaks at log XLa ~ -1.8, but r-process-enhanced stars ([Eu/Fe] > 0.7) have distinctly higher lanthanide fractions; log XLa > -1.5. We review observations of GW170817 and find general consensus that the total log XLa = -2.2 +/- 0.5, somewhat lower than the typical metal-poor star and inconsistent with the most highly r-enhanced stars. For neutron star mergers to remain viable as the dominant r-process site, future kilonova observations should be preferentially lanthanide-rich (including a population of ~10% with log XLa > -1.5). These high-XLa kilonovae may be fainter and more rapidly evolving than GW170817, posing a challenge for discovery and follow-up observations. Both optical and (mid-)infrared observations will be required to robustly constrain kilonova lanthanide fractions. If such high-XLa kilonovae are not found in the next few years, that likely implies that the stars with the highest r-process enhancements have a different origin for their r-process elements.

arXiv commentApJ accepted after minor revisions. 18 pages + appendices, 8 figures, 5 tables. See Figure 5 for summary

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