English (United Kingdom)

https://curated-unify.zendy.io/wp-json/zendy-region/v1/featured_content/oa?rat=en

https://curated-unify.zendy.io/wp-json/zendy-region/v1/highlighted_journal/

Zendy Plus

Presents the access of premium content as premium feature

Premium Content

Presents the keyphrase highlighting as premium feature

Keyphrase Highlighting

Presents the summarisation as premium feature

Summarisation

Insights

Presents the pdf analysis as premium feature

PDF Analysis

Presents the zaia usage as premium feature

ZAIA

Zendy Tools

Zendy Open

Simulations of neutron star-black hole (NSBH) binaries generally considerblack holes with masses in the range $(5-10)M_\odot$, where we expect to findmost stellar mass black holes. The existence of lower mass black holes,however, cannot be theoretically ruled out. Low-mass black holes in binarysystems with a neutron star companion could mimic neutron star-neutron (NSNS)binaries, as they power similar gravitational wave (GW) and electromagnetic(EM) signals. To understand the differences and similarities between NSNSmergers and low-mass NSBH mergers, numerical simulations are required. Here, weperform a set of simulations of low-mass NSBH mergers, including systemscompatible with GW170817. Our simulations use a composition and temperaturedependent equation of state (DD2) and approximate neutrino transport, but nomagnetic fields. We find that low-mass NSBH mergers produce remnant diskssignificantly less massive than previously expected, and consistent with thepost-merger outflow mass inferred from GW170817 for moderately asymmetric massratio. The dynamical ejecta produced by systems compatible with GW170817 isnegligible except if the mass ratio and black hole spin are at the edge of theallowed parameter space. That dynamical ejecta is cold, neutron-rich, andsurprisingly slow for ejecta produced during the tidal disruption of a neutronstar : $v\sim (0.1-0.15)c$. We also find that the final mass of the remnantblack hole is consistent with existing analytical predictions, while the finalspin of that black hole is noticeably larger than expected -- up to $\chi_{\rmBH}=0.84$ for our equal mass case.

Numerical simulations of neutron star-black hole binaries in the near-equal-mass regime