Formation of counter-rotating and highly eccentric massive black hole binaries in galaxy mergers

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dc.contributor.authorNasim, Imran Tariq
dc.contributor.authorPetrovich, Cristobal
dc.contributor.authorNasim, Adam
dc.contributor.authorDosopoulou, Fani
dc.contributor.authorAntonini, Fabio
dc.date.accessioned2025-01-20T23:53:20Z
dc.date.available2025-01-20T23:53:20Z
dc.date.issued2021
dc.description.abstractSupermassive black hole (SMBH) binaries represent the main target for missions such as the Laser Interferometer Space Antenna and Pulsar Timing Arrays. The understanding of their dynamical evolution prior to coalescence is therefore crucial to improving detection strategies and for the astrophysical interpretation of the gravitational wave data. In this paper, we use high-resolution N-body simulations to model the merger of two equal-mass galaxies hosting a central SMBH. In our models, all binaries are initially prograde with respect to the galaxy sense of rotation. But, binaries that form with a high eccentricity, e greater than or similar to 0.7, quickly reverse their sense of rotation and become almost perfectly retrograde at the moment of binary formation. The evolution of these binaries proceeds towards larger eccentricities, as expected for a binary hardening in a counter-rotating stellar distribution. Binaries that form with lower eccentricities remain prograde and at comparatively low eccentricities. We study the origin of the orbital flip by using an analytical model that describes the early stages of binary evolution. This model indicates that the orbital plane flip is due to the torque from the triaxial background mass distribution that naturally arises from the galactic merger process. Our results imply the existence of a population of SMBH binaries with a high eccentricity and could have significant implications for the detection of the gravitational wave signal emitted by these systems.
dc.fuente.origenWOS
dc.identifier.doi10.1093/mnras/stab351
dc.identifier.eissn1365-2966
dc.identifier.issn0035-8711
dc.identifier.urihttps://doi.org/10.1093/mnras/stab351
dc.identifier.urihttps://repositorio.uc.cl/handle/11534/94955
dc.identifier.wosidWOS:000641987400033
dc.issue.numero1
dc.language.isoen
dc.pagina.final510
dc.pagina.inicio498
dc.revistaMonthly notices of the royal astronomical society
dc.rightsacceso restringido
dc.subjectblack hole physics
dc.subjectgravitational waves
dc.subjectmethods: numerical
dc.subjectgalaxies: interactions
dc.subjectgalaxies: kinematics and dynamics
dc.subjectgalaxies: nuclei
dc.titleFormation of counter-rotating and highly eccentric massive black hole binaries in galaxy mergers
dc.typeartículo
dc.volumen503
sipa.indexWOS
sipa.trazabilidadWOS;2025-01-12
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