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/

Global: Zendy Plus annual

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

Global: Zendy Tools annual

Global: Zendy Free Plan

Global: Zendy Tools monthly

Global: Zendy Plus monthly

Black hole-neutron star mergers resulting in the disruption of the neutronstar and the formation of an accretion disk and/or the ejection of unboundmaterial are prime candidates for the joint detection of gravitational-wave andelectromagnetic signals when the next generation of gravitational-wavedetectors comes online. However, the disruption of the neutron star and theproperties of the post-merger remnant are very sensitive to the parameters ofthe binary. In this paper, we study the impact of the radius of the neutronstar and the alignment of the black hole spin for systems within the range ofmass ratio currently deemed most likely for field binaries (M_BH ~ 7 M_NS) andfor black hole spins large enough for the neutron star to disrupt (J/M^2=0.9).We find that: (i) In this regime, the merger is particularly sensitive to theradius of the neutron star, with remnant masses varying from 0.3M_NS to 0.1M_NSfor changes of only 2 km in the NS radius; (ii) 0.01-0.05M_sun of unboundmaterial can be ejected with kinetic energy >10^51 ergs, a significant increasecompared to low mass ratio, low spin binaries. This ejecta could powerdetectable optical and radio afterglows. (iii) Only a small fraction (<3%) ofthe Advanced LIGO events in this parameter range have gravitational-wavesignals which could offer constraints on the equation of state of the neutronstar. (iv) A misaligned black hole spin works against disk formation, with lessneutron star material remaining outside of the black hole after merger, and alarger fraction of that material remaining in the tidal tail instead of theforming accretion disk. (v) Large kicks (v>300 km/s) can be given to the finalblack hole as a result of a precessing BHNS merger, when the disruption of theneutron star occurs just outside or within the innermost stable sphericalorbit.

Black hole-neutron star mergers at realistic mass ratios: Equation of state and spin orientation effects