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

Detections of gravitational waves (GWs) may soon uncover the signal from thecoalescence of a black hole - neutron star (BHNS) binary, that is expected tobe accompanied by an electromagnetic (EM) signal. In this paper, we present acomposite semi-analytical model to predict the properties of the expected EMcounterpart from BHNS mergers, focusing on the kilonova emission and on thegamma-ray burst afterglow. Four main parameters rule the properties of the EMemission: the NS mass $M_\mathrm{NS}$, its tidal deformability$\Lambda_\mathrm{NS}$, the BH mass and spin. Only for certain combinations ofthese parameters an EM counterpart is produced. Here we explore the parameterspace, and construct light curves, analysing the dependence of the EM emissionon the NS mass and tidal deformability. Exploring the NS parameter spacelimiting to $M_\mathrm{NS}-\Lambda_\mathrm{NS}$ pairs described by a physicallymotivated equations of state (EoS), we find that the brightest EM counterpartsare produced in binaries with low mass NSs (fixing the BH properties and theEoS). Using constraints on the NS EoS from GW170817, our modeling shows thatthe emission falls in a narrow range of absolute magnitudes. Within the rangeof explored parameters, light curves and peak times are not dissimilar to thosefrom NSNS mergers, except in the B band. The lack of an hyper/supra-massive NSin BHNS coalescences causes a dimming of the blue kilonova emission in absenceof the neutrino interaction with the ejecta.

Electromagnetic counterparts of black hole-neutron star mergers: dependence on the neutron star properties