Bulletin of the American Physical Society
APS April Meeting 2016
Volume 61, Number 6
Saturday–Tuesday, April 16–19, 2016; Salt Lake City, Utah
Session X14: Compact Binary Mergers: Rates, Populations, Waveforms, and Tidal Effects |
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Sponsoring Units: GGR DAP Chair: Tanja Hinderer, Max Planck Institute for Gravitational Physics Room: 251AB |
Tuesday, April 19, 2016 10:45AM - 10:57AM |
X14.00001: ABSTRACT WITHDRAWN |
Tuesday, April 19, 2016 10:57AM - 11:09AM |
X14.00002: Expected Bounds on Compact Binary Coalescence Rates from LIGO Observations Laura Sampson The Advanced LIGO detectors have recently completed their first observing run, with a sensitive spacetime volume over 27 times larger than the initial LIGO configuration. In this talk we will examine the expected bounds on compact binary coalescence rates from O1 observations, and discuss the corresponding impact on astrophysical models. [Preview Abstract] |
Tuesday, April 19, 2016 11:09AM - 11:21AM |
X14.00003: Variance in binary stellar population synthesis Katelyn Breivik, Shane L. Larson In the years preceding LISA, Milky Way compact binary population simulations can be used to inform the science capabilities of the mission. Galactic population simulation efforts generally focus on high fidelity models that require extensive computational power to produce a single simulated population for each model. Each simulated population represents an incomplete sample of the functions governing compact binary evolution, thus introducing variance from one simulation to another. We present a rapid Monte Carlo population simulation technique that can simulate thousands of populations in less than a week, thus allowing a full exploration of the variance associated with a binary stellar evolution model. [Preview Abstract] |
Tuesday, April 19, 2016 11:21AM - 11:33AM |
X14.00004: Beyond the Horizon Distance: LIGO-Virgo can Boost Gravitational-Wave Detection Rates by Exploiting the Mass Distribution of Neutron Star and Black Hole Binaries Zsuzsa Marka, Imre Bartos, Szabolcs Marka We explore the advantage of focusing on regions of the parameter space in gravitational-wave searches for the binary mergers of neutron stars and black holes. For neutron star binaries, we show that taking advantage of their narrow observed mass distribution could improve detection rates, in some cases by more than 50%. A reduced template bank can also represent significant improvement in technical cost. We present a detailed search method using binary mass distribution to incorporate information on the mass distribution. [Preview Abstract] |
Tuesday, April 19, 2016 11:33AM - 11:45AM |
X14.00005: Binary Black Holes from Globular Clusters in the Advanced LIGO Era Carl Rodriguez, Sourav Chatterjee, Fred Rasio With Advanced LIGO now collecting data, the field of gravitational-wave astronomy is poised to open a new window into the universe; but to look though that window, we must be able to link gravitational-wave observations to detailed astrophysical models. We have generated a collection of globular cluster models with all the relevant physics, such as two-body relaxation, binary interactions, and stellar evolution. I will show how the global properties of a cluster determine the properties of its binary black hole population. I will also describe the masses, mass ratios, eccentricities, and cosmological merger rates for detectible binaries predicted by our models. Finally, I will show that, because binaries in clusters are formed dynamically, our results are insensitive to the assumptions and uncertainties associated with binary stellar evolution. [Preview Abstract] |
Tuesday, April 19, 2016 11:45AM - 11:57AM |
X14.00006: Error analysis of numerical gravitational waveforms from coalescing binary black holes Heather Fong, Tony Chu, Prayush Kumar, Harald Pfeiffer, Michael Boyle, Daniel Hemberger, Lawrence Kidder, Mark Scheel, Bela Szilagyi The Advanced Laser Interferometer Gravitational-wave Observatory (Advanced LIGO) has finished a successful first observation run and will commence its second run this summer. Detection of compact object binaries utilizes matched-filtering, which requires a vast collection of highly accurate gravitational waveforms. This talk will present a set of about 100 new aligned-spin binary black hole simulations. I will discuss their properties, including a detailed error analysis, which demonstrates that the numerical waveforms are sufficiently accurate for gravitational wave detection purposes, as well as for parameter estimation purposes. [Preview Abstract] |
Tuesday, April 19, 2016 11:57AM - 12:09PM |
X14.00007: Accuracy Of Binary Black Hole Waveform Models For Advanced LIGO Prayush Kumar, Heather Fong, Kevin Barkett, Swetha Bhagwat, Nousha Afshari, Tony Chu, Duncan Brown, Geoffrey Lovelace, Harald Pfeiffer, Mark Scheel, Bela Szilagyi Coalescing binaries of compact objects, such as black holes and neutron stars, are the primary targets for gravitational-wave (GW) detection with Advanced LIGO. Accurate modeling of the emitted GWs is required to extract information about the binary source. The most accurate solution to the general relativistic two-body problem is available in numerical relativity (NR), which is however limited in application due to computational cost. Current searches use semi-analytic models that are based in post-Newtonian (PN) theory and calibrated to NR. In this talk, I will present comparisons between contemporary models and high-accuracy numerical simulations performed using the Spectral Einstein Code (SpEC), focusing at the questions: (i) How well do models capture binary's late-inspiral where they lack a-priori accurate information from PN or NR, and (ii) How accurately do they model binaries with parameters outside their range of calibration. These results guide the choice of templates for future GW searches, and motivate future modeling efforts. [Preview Abstract] |
Tuesday, April 19, 2016 12:09PM - 12:21PM |
X14.00008: Accuracy and precision of gravitational-wave models of inspiraling neutron star-black hole binaries with spin: Comparison with matter-free numerical relativity in the low-frequency regime Swetha Bhagwat, Prayush Kumar, Kevin Barkett, Nousha Afshari, Duncan A. Brown, Geoffrey Lovelace, Mark A Scheel, Bela Szilagyi Detection of gravitational wave involves extracting extremely weak signal from noisy data and their detection depends crucially on the accuracy of the signal models. The most accurate models of compact binary coalescence are known to come from solving the Einstein's equation numerically without any approximations. However, this is computationally formidable. As a more practical alternative, several analytic or semi analytic approximations are developed to model these waveforms. However, the work of Nitz et al. (2013) demonstrated that there is disagreement between these models. We present a careful follow up study on accuracies of different waveform families for spinning black-hole neutron star binaries, in context of both detection and parameter estimation and find that SEOBNRv2 to be the most faithful model. Post Newtonian models can be used for detection but we find that they could lead to large parameter bias. [Preview Abstract] |
Tuesday, April 19, 2016 12:21PM - 12:33PM |
X14.00009: Gravitational waves from neutron-star mergers. Jocelyn Read, Torrey Cullen, Eric Flynn, Veronica Lockett-Ruiz, Conner Park, Susan Vong The inspiral and merger of binary neutron stars is expected to provide many signals for Advanced LIGO at design sensitivity. The waveform models currently used to search for and parameterize these signals ignore effects near the merger: as the stars coalesce, the gravitational waves depend additionally on the properties of matter in the core of the stars. In this talk, I will discuss potential systematic error from neglecting these features and present phenomenological waveform models currently being developed to capture the dynamics of merging neutron stars. [Preview Abstract] |
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