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Surface abundance observations of halo stars hint at the occurrence of$r$-process nucleosynthesis at low metallicity ($\rm{[Fe/H]< -3}$), possiblywithin the first $10^8$ yr after the formation of the first stars. Possibleloci of early-Universe $r$-process nucleosynthesis are the ejecta of eitherblack hole--neutron star or neutron star--neutron star binary mergers. Here westudy the effect of the inclination--eccentricity oscillations raised by atertiary (e.g. a star) on the coalescence time scale of the inner compactobject binaries. Our results are highly sensitive to the assumed initialdistribution of the inner binary semi-major axes. Distributions with mostlywide compact object binaries are most affected by the third object, resultingin a strong increase (by more than a factor of 2) in the fraction of fastcoalescences. If instead the distribution preferentially populates very closecompact binaries, general relativistic precession prevents the third body fromincreasing the inner binary eccentricity to very high values. In this lastcase, the fraction of coalescing binaries is increased much less by tertiaries,but the fraction of binaries that would coalesce within $10^8$ yr even withouta third object is already high. Our results provide additional support to thecompact object merger scenario for $r$-process nucleosynthesis.

$r$-process nucleosynthesis in the early Universe through fast mergers of compact binaries in triple systems