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Black hole-neutron star coalescence: effects of the neutron star spin on jet launching and dynamical ejecta mass

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Black hole-neutron star coalescence: effects of the neutron star spin on jet launching and dynamical ejecta mass

dc.contributor.author	Ruiz Meneses, Milton Javier
dc.contributor.author	Paschalidis, Vasileios
dc.contributor.author	Tsokaros, Antonios
dc.contributor.author	Shapiro, Stuart L.
dc.date.accessioned	2023-06-05T07:11:24Z
dc.date.available	2023-06-05T07:11:24Z
dc.date.issued	2020
dc.identifier.citation	Ruiz Meneses, Milton Javier Paschalidis, Vasileios Tsokaros, Antonios Shapiro, Stuart L. 2020 Black hole-neutron star coalescence: effects of the neutron star spin on jet launching and dynamical ejecta mass Physical Review D 102 12 1 16
dc.identifier.uri	https://hdl.handle.net/10550/87686
dc.description.abstract	Black hole-neutron star (BHNS) mergers are thought to be sources of gravitational waves (GWs) with coincident electromagnetic (EM) counterparts. To further probe whether these systems are viable progenitors of short gamma-ray bursts (SGRBs) and kilonovas, and how one may use (the lack of) EM counterparts associated with LIGO/Virgo candidate BHNS GW events to sharpen parameter estimation, we study the impact of neutron star spin in BHNS mergers. Using dynamical spacetime magnetohydrodynamic simulations of BHNSs initially on a quasicircular orbit, we survey configurations that differ in the BH spin (aBH/MBH=0 and 0.75), the NS spin (aNS/MNS=−0.17, 0, 0.23, and 0.33), and the binary mass ratio (q≡MBH:MNS=3∶1 and 5∶1). The general trend we find is that increasing the NS prograde spin increases both the rest mass of the accretion disk onto the remnant black hole, and the rest mass of dynamically ejected matter. By a time Δt∼3500-5500M∼88-138(MNS/1.4 M⊙) ms after the peak gravitational-wave amplitude, a magnetically driven jet is launched only for q=3∶1 regardless of the initial NS spin. The lifetime of the jets [Δt∼0.5-0.8(MNS/1.4 M⊙) s] and their outgoing Poynting luminosity [LPoyn∼1051.5±0.5 erg/s] are consistent with typical SGRBs' luminosities and expectations from the Blandford-Znajek mechanism. By the time we terminate our simulations, we do not observe either an outflow or a large-scale magnetic-field collimation for the other systems we consider. The mass range of dynamically ejected matter is 10−4.5-10−2(MNS/1.4 M⊙) M⊙, which can power kilonovas with peak bolometric luminosities Lknova∼1040-1041.4 erg/s with rise times ≲6.5 h and potentially detectable by the LSST.
dc.language.iso	eng
dc.relation.ispartof	Physical Review D, 2020, vol. 102, num. 12, p. 1-16
dc.subject	Astronomia
dc.subject	Astrofísica
dc.title	Black hole-neutron star coalescence: effects of the neutron star spin on jet launching and dynamical ejecta mass
dc.type	journal article
dc.date.updated	2023-06-05T07:11:26Z
dc.identifier.doi	10.1103/PhysRevD.102.124077
dc.identifier.idgrec	160094
dc.rights.accessRights	open access