The possible electromagnetic counterparts of the first high-probability NSBH merger LIGO/Virgo S190814bv

Hao Wei,Minzi Feng

Figure 1. Panel (I) corresponds to case (2a) of [29], namely the neutron star N as the mirror for GWs is much closer to the observer O on Earth, with luminosity distance dON ≪ dSN. Panels (II) and (III) correspond to cases (3a) and (3b) of [29], namely the neutron star N as the mirror for GWs is much closer to the GW source S, with luminosity distance dSN ≪ dON. S′ is the mirror image of the GW source S. All plots are not to scale. See the text and [29] for details.