Bulletin of the American Physical Society
APS April Meeting 2014
Volume 59, Number 5
Saturday–Tuesday, April 5–8, 2014; Savannah, Georgia
Session E11: Invited Session: Compact Binaries and Gravitational Waves: Simulations, Templates and Interpretation |
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Sponsoring Units: GGR Chair: Frans Pretorius, Princeton University Room: Oglethorpe Auditorium |
Saturday, April 5, 2014 3:30PM - 4:06PM |
E11.00001: Numerical simulations of merging black holes for gravitational-wave astronomy Invited Speaker: Geoffrey Lovelace Gravitational waves from merging binary black holes (BBHs) are among the most promising sources for current and future gravitational-wave detectors. Accurate models of these waves are necessary to maximize the number of detections and our knowledge of the waves' sources; near the time of merger, the waves can only be computed using numerical-relativity simulations. For optimal application to gravitational-wave astronomy, BBH simulations must achieve sufficient accuracy and length, and all relevant regions of the BBH parameter space must be covered. While great progress toward these goals has been made in the almost nine years since BBH simulations became possible, considerable challenges remain. In this talk, I will discuss current efforts to meet these challenges, and I will present recent BBH simulations produced using the Spectral Einstein Code, including a catalog of publicly available gravitational waveforms [black-holes.org/waveforms]. I will also discuss simulations of merging black holes with high mass ratios and with spins nearly as fast as possible, the most challenging regions of the BBH parameter space. [Preview Abstract] |
Saturday, April 5, 2014 4:06PM - 4:42PM |
E11.00002: Reduced Order Modeling in General Relativity Invited Speaker: Manuel Tiglio Reduced Order Modeling is an emerging yet fast developing filed in gravitational wave physics. The main goals are to enable fast modeling and parameter estimation of any detected signal, along with rapid matched filtering detecting. I will focus on the first two. Some accomplishments include being able to replace, with essentially no lost of physical accuracy, the original models with surrogate ones (which are not effective ones, that is, they do not simplify the physics but go on a very different track, exploiting the particulars of the waveform family under consideration and state of the art dimensional reduction techniques) which are very fast to evaluate. For example, for EOB models they are at least around 3 orders of magnitude faster than solving the original equations, with physically equivalent results. For numerical simulations the speedup is at least 11 orders of magnitude. For parameter estimation our current numbers are about bringing $\sim$100 days for a single SPA inspiral binary neutron star Bayesian parameter estimation analysis to under a day. More recently, it has been shown that the full precessing problem for, say, 200 cycles, can be represented, through some new ideas, by a remarkably compact set of carefully chosen reduced basis waveforms ($\sim$10-100, depending on the accuracy requirements). I will highlight what I personally believe are the challenges to face next in this subarea of GW physics and where efforts should be directed. \\[4pt] This talk will summarize work in collaboration with: Harbir Antil (GMU), Jonathan Blackman (Caltech), Priscila Canizares (IoA, Cambridge, UK), Sarah Caudill (UWM), Jonathan Gair (IoA. Cambridge. UK), Scott Field (UMD), Chad R. Galley (Caltech), Frank Herrmann (Germany), Han Hestahven (EPFL, Switzerland), Jason Kaye (Brown, Stanford \& Courant). Evan Ochsner (UWM), Ricardo Nochetto (UMD), Vivien Raymond (LIGO, Caltech), Rory Smith (LIGO, Caltech) Bela Ssilagyi (Caltech) and MT (UMD \& Caltech). [Preview Abstract] |
Saturday, April 5, 2014 4:42PM - 5:18PM |
E11.00003: Three-Hair Relations, Orbital Motion and Gravitational Waves from Neutron Star Binaries Invited Speaker: Nicolas Yunes Neutron stars are one of the most relativistic objects in the Universe. The gravitational waves they emit when two of them spiral into each other and merge are one of the primary targets of ground-based gravitational wave observatories, such as LIGO and Virgo. In this talk, I will describe a new set of three-hair relations (analogous to the no-hair relations of black holes) that prescribe all multipole moments of the external gravitational field of neutron stars in terms of only the mass, the spin angular momentum and the quadrupole moment. I will then describe how these relations allow us to construct more accurate gravitational waveform for neutron star inspirals. Such waveforms may allow us to better measure certain combinations of the neutron star's individual spins, as well as the tidal Love number, from which one may be able to infer the neutron star equation of state. [Preview Abstract] |
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