Bulletin of the American Physical Society
APS April Meeting 2017
Volume 62, Number 1
Saturday–Tuesday, January 28–31, 2017; Washington, DC
Session X2: Gravitational Wave Source Modeling |
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Sponsoring Units: DGRAV Chair: Reed Essick, Massachusetts Institute of Technology Room: Maryland B |
Tuesday, January 31, 2017 10:45AM - 10:57AM |
X2.00001: Kicked waveforms: prospects for direct detection of black hole recoils Davide Gerosa, Christopher Moore Generic black hole binaries radiate gravitational waves anisotropically, imparting a recoil, or kick, velocity to the merger remnant. If a component of the kick along the line of sight is present, gravitational waves emitted during the final orbits and merger will be gradually Doppler shifted as the kick builds up. We develop a simple prescription to capture this effect in existing waveform models, showing that future gravitational wave experiments will be able to perform direct measurements, not only of the black hole kick velocity, but also of its accumulation profile. In particular, the eLISA space mission will measure supermassive black hole kick velocities as low as 500 km/s, which are expected to be a common outcome of black hole binary coalescence following galaxy mergers. Black hole kicks thus constitute a promising new observable in the growing field of gravitational wave astronomy. [Preview Abstract] |
Tuesday, January 31, 2017 10:57AM - 11:09AM |
X2.00002: Remnant of binary black-hole mergers: New simulations, peak luminosity and hangup studies Carlos Lousto, James Healy We present the results of 61 new simulations of nonprecessing spinning
black hole binaries with mass ratios $q=m_1/m_2$ in the range
$1\leq q\leq1/3$ and individual spins covering the parameter space
$-1<\alpha_{1,2}<1$. We additionally perform 10
new simulations of nonspinning black hole binaries with mass ratios
covering the range $1/10 |
Tuesday, January 31, 2017 11:09AM - 11:21AM |
X2.00003: Development of accurate waveform models for eccentric compact binaries with numerical relativity simulations Eliu Huerta, Bhanu Agarwal, Alvin Chua, Daniel George, Roland Haas, Ian Hinder, Prayush Kumar, Christopher Moore, Harald Pfeiffer We recently constructed an inspiral-merger-ringdown (IMR) waveform model to describe the dynamical evolution of compact binaries on eccentric orbits (https://arxiv.org/abs/1609.05933), and used this model to constrain the eccentricity with which the gravitational wave transients currently detected by LIGO could be effectively recovered with banks of quasi-circular templates. We now present the second generation of this model, which is calibrated using a large catalog of eccentric numerical relativity simulations. We discuss the new features of this model, and show that its enhance accuracy makes it a powerful tool to detect eccentric signals with LIGO. [Preview Abstract] |
Tuesday, January 31, 2017 11:21AM - 11:33AM |
X2.00004: A complete waveform model for compact binaries on eccentric orbits Daniel George, Eliu Huerta, Prayush Kumar, Bhanu Agarwal, Hsi-Yu Schive, Harald Pfeiffer, Tony Chu, Michael Boyle, Daniel Hemberger, Lawrence Kidder, Mark Scheel, Bela Szilagyi We present a time domain waveform model that describes the inspiral, merger and ringdown of compact binary systems whose components are non-spinning, and which evolve on orbits with low to moderate eccentricity (arXiv:1609.05933). We show that this inspiral-merger-ringdown waveform model reproduces the effective-one-body model for black hole binaries with mass-ratios between 1 to 15 in the zero eccentricity limit over a wide range of the parameter space under consideration. We use this model to show that the gravitational wave transients GW150914 and GW151226 can be effectively recovered with template banks of quasicircular, spin-aligned waveforms if the eccentricity e0 of these systems when they enter the aLIGO band at a gravitational wave frequency of 14 Hz satisfies \(e_0^{\rm GW150914}\leq0.15\) and \(e_0^{\rm GW151226}\leq0.1\). [Preview Abstract] |
Tuesday, January 31, 2017 11:33AM - 11:45AM |
X2.00005: Secular evolution of very eccentric, inclined orbits around a supermassive rotating black hole Clifford Will, Matthew Maitra We analyze the secular evolution of the highly eccentric, inclined orbit of a star or black hole in the field of a rotating massive Kerr black hole. Such orbits, with $1-e$ ranging from $10^{-2}$ to $10^{-6}$ may be the end result of a process of stellar interactions in a dense nuclear star cluster surrounding the black hole, leading to extreme-mass ratio inspirals (EMRIs). The calculations are done in post-Newtonian (PN) theory, through 3PN order in the conservative sector, including spin-orbit, quadrupolar and (spin)$^2$ terms from the Kerr geometry, and through 4.5PN order, including 4PN spin-orbit contributions, in the radiation reaction sector. We also incorporate an accurate criterion for capture of the body by the rotating black hole for arbitrary inclinations. For a range of initial values of the body’s semi-major axis, eccentricity and inclination, we determine the time and number of orbits until plunge and the final orbital eccentricity. We also estimate the gravitational-wave frequency and energy flux at the final plunge, as a function of the orbital inclination. [Preview Abstract] |
Tuesday, January 31, 2017 11:45AM - 11:57AM |
X2.00006: Analytic gravitational waveforms for generic precessing compact binaries Katerina Chatziioannou, Antoine Klein, Neil Cornish, Nicolas Yunes Gravitational waves from compact binaries are subject to amplitude and phase modulations arising from interactions between the angular momenta of the system. Failure to account for such spin-precession effects in gravitational wave data analysis could hinder detection and completely ruin parameter estimation. In this talk I will describe the construction of closed-form, frequency-domain waveforms for fully-precessing, quasi-circular binary inspirals. The resulting waveforms can model spinning binaries of arbitrary spin magnitudes, spin orientations, and masses during the inspiral phase. I will also describe ongoing efforts to extend these inspiral waveforms to the merger and ringdown phases. [Preview Abstract] |
Tuesday, January 31, 2017 11:57AM - 12:09PM |
X2.00007: Gravitational waves from compact binaries in scalar-tensor gravity to second post-Newtonian order Anna Heffernan, Ryan Lang, Clifford Will Testing alternative theories of gravity in the strong-field gravitational-wave regime can be an important complement to solar-system tests. A leading alternative is the class of scalar-tensor theories; for binary systems of compact objects, equations of motion and the tensor waveform and energy flux have been derived through second post-Newtonian (2PN) order. However, because the scalar field in these theories admits dipole gravitational radiation, a calculation of the scalar contribution to the energy flux requires calculating the scalar field and the equations of motion to 3PN order. We report on progress toward completing this calculation and obtaining waveforms to 2PN order, suitable for gravitational-wave data analysis. [Preview Abstract] |
Tuesday, January 31, 2017 12:09PM - 12:21PM |
X2.00008: Detectability of the nonlinear gravitational wave memory with second and third-generation ground-based detectors Marc Favata, Emanuele Berti Gravitational wave memory refers to a non-oscillating component of a gravitational wave signal. In principle, all gravitational-wave sources have a memory component. The largest sources of memory waves are the merger of two black holes. These produce the so-called nonlinear or Blanchet-Damour-Christodoulou memory. We will discuss the prospects for detecting the nonlinear memory with current and third-generation ground-based interferometers. [Preview Abstract] |
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