The Experts below are selected from a list of 261 Experts worldwide ranked by ideXlab platform
Yosef Zlochower - One of the best experts on this subject based on the ideXlab platform.
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Modeling gravitational recoil from precessing highly spinning unequal-mass black-hole binaries
Physical Review D, 2009Co-Authors: Carlos O. Lousto, Yosef ZlochowerAbstract:We measure the gravitational recoil for unequal-mass black-hole binary mergers, with the larger black hole having intrinsic spin $a/{m}^{H}=0.8$, and the smaller black hole nonspinning. We choose our configurations such that, initially, the spins lie on the Orbital Plane. The spin and Orbital Plane precess significantly (we introduce a technique to identify the Orbital Plane at merger), and we find that the out-of Plane recoil (i.e. the recoil perpendicular to the Orbital Plane around merger) varies as ${\ensuremath{\eta}}^{2}/(1+q)$, in agreement with our previous prediction, based on the post-Newtonian scaling.
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Large Merger Recoils and Spin Flips from Generic Black Hole Binaries
The Astrophysical Journal, 2007Co-Authors: Manuela Campanelli, Carlos O. Lousto, Yosef Zlochower, David MerrittAbstract:We report the first results from the evolution of generic black hole binaries, i.e., binaries containing unequal-mass black holes with misaligned spins. Our configuration, which has a mass ratio of 2?:?1, consists of an initially nonspinning hole orbiting a larger, rapidly spinning hole (specific spin a/m = 0.885), with the spin direction oriented -45? with respect to the Orbital Plane. We track the inspiral and merger for ~2 orbits and find that the remnant receives a substantial kick of 454 km s-1, more than twice as large as the maximum kick from nonspinning binaries. The remnant spin direction is flipped by 103? with respect to the initial spin direction of the larger hole. We performed a second run with antialigned spins, a/m = ?0.5 lying in the Orbital Plane that produces a kick of ~1830 km s-1 off the Orbital Plane. This value scales to nearly 4000 km s-1 for maximally spinning holes. Such a large recoil velocity opens up the possibility that a merged binary can be ejected even from the nucleus of a massive host galaxy.
Noam Soker - One of the best experts on this subject based on the ideXlab platform.
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Shaping Planetary nebulae with jets in inclined triple stellar systems
Monthly Notices of the Royal Astronomical Society, 2017Co-Authors: Muhammad Akashi, Noam SokerAbstract:We conduct three-dimensional hydrodynamical simulations of two opposite jets launched obliquely to the Orbital Plane around an asymptotic giant branch (AGB) star and within its dense wind, and demonstrate the formation of a `messy' Planetary nebula (PN), namely, a PN lacking any type of symmetry (highly irregular). In building the initial conditions we assume that a tight binary system orbits the AGB star, and that the Orbital Plane of the tight binary system is inclined to the Orbital Plane of the binary system and the AGB star (the triple system Plane). We further assume that the accreted mass on to the tight binary system forms an accretion disk around one of the stars, and that the Plane of the disk is tilted to the Orbital Plane of the triple system. The highly asymmetrical and filamentary structure that we obtain support the notion that messy PNe might be shaped by triple stellar systems.
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Shaping Planetary nebulae with jets in inclined triple stellar systems
Proceedings of the International Astronomical Union, 2016Co-Authors: Muhammad Akashi, Noam SokerAbstract:AbstractWe conduct three-dimensional hydrodynamical simulations of two opposite jets launched obliquely to the Orbital Plane around an asymptotic giant branch (AGB) star and within its dense wind, and demonstrate the formation of a ‘messy’ Planetary nebula (PN), namely, a PN lacking any type of symmetry (highly irregular). In building the initial conditions we assume that a tight binary system orbits the AGB star, and that the Orbital Plane of the tight binary system is inclined to the Orbital Plane of binary system and the AGB star. We further assume that the accreted mass onto the tight binary system forms an accretion disk around one of the stars, and that the Plane of the disk is in between the two Orbital Planes. The highly asymmetrical lobes that we obtain support the notion that messy PNe might be shaped by triple stellar systems.
Carlos O. Lousto - One of the best experts on this subject based on the ideXlab platform.
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Modeling gravitational recoil from precessing highly spinning unequal-mass black-hole binaries
Physical Review D, 2009Co-Authors: Carlos O. Lousto, Yosef ZlochowerAbstract:We measure the gravitational recoil for unequal-mass black-hole binary mergers, with the larger black hole having intrinsic spin $a/{m}^{H}=0.8$, and the smaller black hole nonspinning. We choose our configurations such that, initially, the spins lie on the Orbital Plane. The spin and Orbital Plane precess significantly (we introduce a technique to identify the Orbital Plane at merger), and we find that the out-of Plane recoil (i.e. the recoil perpendicular to the Orbital Plane around merger) varies as ${\ensuremath{\eta}}^{2}/(1+q)$, in agreement with our previous prediction, based on the post-Newtonian scaling.
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Large Merger Recoils and Spin Flips from Generic Black Hole Binaries
The Astrophysical Journal, 2007Co-Authors: Manuela Campanelli, Carlos O. Lousto, Yosef Zlochower, David MerrittAbstract:We report the first results from the evolution of generic black hole binaries, i.e., binaries containing unequal-mass black holes with misaligned spins. Our configuration, which has a mass ratio of 2?:?1, consists of an initially nonspinning hole orbiting a larger, rapidly spinning hole (specific spin a/m = 0.885), with the spin direction oriented -45? with respect to the Orbital Plane. We track the inspiral and merger for ~2 orbits and find that the remnant receives a substantial kick of 454 km s-1, more than twice as large as the maximum kick from nonspinning binaries. The remnant spin direction is flipped by 103? with respect to the initial spin direction of the larger hole. We performed a second run with antialigned spins, a/m = ?0.5 lying in the Orbital Plane that produces a kick of ~1830 km s-1 off the Orbital Plane. This value scales to nearly 4000 km s-1 for maximally spinning holes. Such a large recoil velocity opens up the possibility that a merged binary can be ejected even from the nucleus of a massive host galaxy.
Matthew J Holman - One of the best experts on this subject based on the ideXlab platform.
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Discovery of a New Retrograde Trans-Neptunian Object: Hint of a Common Orbital Plane for Low Semimajor Axis, High-inclination TNOs and Centaurs
The Astrophysical Journal, 2016Co-Authors: Ying-tung Chen, Matthew J Holman, Hsing Wen Lin, Matthew J. Payne, Wesley C. Fraser, Pedro Lacerda, Wen-ping Chen, Rolf-peter Kudritzki, Robert JedickeAbstract:Although the majority of Centaurs are thought to have originated in the scattered disk, with the high-inclination members coming from the Oort cloud, the origin of the high inclination component of trans-Neptunian objects (TNOs) remains uncertain. We report the discovery of a retrograde TNO, which we nickname "Niku", detected by the Pan-STARRS 1 Outer Solar System Survey. Our numerical integrations show that the Orbital dynamics of Niku are very similar to that of 2008 KV$_{42}$ (Drac), with a half-life of $\sim 500$ Myr. Comparing similar high inclination TNOs and Centaurs ($q > 10$ AU, $a 60^\circ$), we find that these objects exhibit a surprising clustering of ascending node, and occupy a common Orbital Plane. This Orbital configuration has high statistical significance: 3.8-$\sigma$. An unknown mechanism is required to explain the observed clustering. This discovery may provide a pathway to investigate a possible reservoir of high-inclination objects.
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discovery of a new retrograde trans neptunian object hint of a common Orbital Plane for low semi major axis high inclination tnos and centaurs
arXiv: Earth and Planetary Astrophysics, 2016Co-Authors: Ying-tung Chen, Matthew J Holman, Hsing Wen Lin, Matthew J. Payne, Wesley C. Fraser, Pedro Lacerda, Wen-ping Chen, Rolf-peter Kudritzki, Robert Jedicke, R J WainscoatAbstract:Although the majority of Centaurs are thought to have originated in the scattered disk, with the high-inclination members coming from the Oort cloud, the origin of the high inclination component of trans-Neptunian objects (TNOs) remains uncertain. We report the discovery of a retrograde TNO, which we nickname "Niku", detected by the Pan-STARRS 1 Outer Solar System Survey. Our numerical integrations show that the Orbital dynamics of Niku are very similar to that of 2008 KV$_{42}$ (Drac), with a half-life of $\sim 500$ Myr. Comparing similar high inclination TNOs and Centaurs ($q > 10$ AU, $a 60^\circ$), we find that these objects exhibit a surprising clustering of ascending node, and occupy a common Orbital Plane. This Orbital configuration has high statistical significance: 3.8-$\sigma$. An unknown mechanism is required to explain the observed clustering. This discovery may provide a pathway to investigate a possible reservoir of high-inclination objects.
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chaotic variations in the eccentricity of the Planet orbiting 16 cygni b
Nature, 1997Co-Authors: Matthew J Holman, Jihad Touma, Scott TremaineAbstract:The Planet recently discovered1 orbiting the star 16 Cyg B has the largest eccentricity (e= 0.67) of any known Planet. Planets that form in circumstellar disks are expected to have nearly circular orbits, although gravitational interactions in a system of two or more Planets could generate high-eccentricity orbits2,3. Here we suggest that the eccentric orbit of 16 Cyg Bb arises from gravitational interactions with the distant companion star, 16 Cyg A. Assuming that 16 Cyg Bb formed in a nearly circular orbit, with the Orbital Plane inclined between 45° and 135° to the Orbital Plane of 16 Cyg A, and that there are no other Planets with a mass similar to that of Jupiter within 30 astronomical units (AU, the average distance between the Earth and the Sun), then 16 Cyg Bb will oscillate between low-eccentricity and high-eccentricity orbits. The transitions between these orbits should occur every 107–109 years, with the Planet spending up to 35 per cent of its lifetime with an eccentricity e> 0.6. These results imply that Planetary orbits in binary stellar systems commonly experience periods of high eccentricity and dynamical chaos, and that such Planets may occasionally collide with the primary star.
David Merritt - One of the best experts on this subject based on the ideXlab platform.
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Large Merger Recoils and Spin Flips from Generic Black Hole Binaries
The Astrophysical Journal, 2007Co-Authors: Manuela Campanelli, Carlos O. Lousto, Yosef Zlochower, David MerrittAbstract:We report the first results from the evolution of generic black hole binaries, i.e., binaries containing unequal-mass black holes with misaligned spins. Our configuration, which has a mass ratio of 2?:?1, consists of an initially nonspinning hole orbiting a larger, rapidly spinning hole (specific spin a/m = 0.885), with the spin direction oriented -45? with respect to the Orbital Plane. We track the inspiral and merger for ~2 orbits and find that the remnant receives a substantial kick of 454 km s-1, more than twice as large as the maximum kick from nonspinning binaries. The remnant spin direction is flipped by 103? with respect to the initial spin direction of the larger hole. We performed a second run with antialigned spins, a/m = ?0.5 lying in the Orbital Plane that produces a kick of ~1830 km s-1 off the Orbital Plane. This value scales to nearly 4000 km s-1 for maximally spinning holes. Such a large recoil velocity opens up the possibility that a merged binary can be ejected even from the nucleus of a massive host galaxy.
