Bulletin of the American Physical Society
APS April Meeting 2019
Volume 64, Number 3
Saturday–Tuesday, April 13–16, 2019; Denver, Colorado
Session D17: Binary Black Hole Mergers and Core-Collapse Supernovae: Modeling in the Multimessenger Era |
Hide Abstracts |
Sponsoring Units: DAP DGRAV Chair: Zach Etienne, West Virginia University Room: Sheraton Grand Ballroom II |
Saturday, April 13, 2019 3:30PM - 3:42PM |
D17.00001: Magnetic-Field and Matter Distribution Dependence of EM Emission during Supermassive Binary Black Hole Mergers Bernard J Kelly, Zach B Etienne, Jeremy Schnittman, John G Baker, Geoffrey S Ryan, Scott C Noble Black-hole binary (BHB) mergers provide a prime source for current and future interferometric gravitational-wave observatories. Massive BHB mergers may often take place in plasma-rich environments, leading to the possibility of a concurrent electromagnetic signal observable by traditional astronomical facilities. However, many critical questions about the generation of such counterparts remain unanswered. In Kelly et al. (2017) [PRD 96:123003], we found a universal form for the time-evolving Poynting luminosity from such systems immersed in initially uniformly magnetized plasma, and demonstrated that after a settling time, this luminosity is relatively insensitive to the initial magnetic field strength. Here, we extend the work of Kelly et al. (2017) to investigate the dependence of the classical Poynting luminosity on variations in the initial magnetic field and matter distribution in the vicinity of the binary. |
Saturday, April 13, 2019 3:42PM - 3:54PM |
D17.00002: Effects of Inner Torque and Dissipation Profiles on the Spectra and Structure of Accretion Disks Theodore Dezen, Bryan Flores, Noah Egger We present numerical spectral and vertical structure calculations appropriate for near-Eddington luminosity, radiation pressure dominated accretion disks around stellar mass black holes. We cover a wide range of black hole spins, and incorporate several dissipation profiles based on first-principles three-dimensional MHD disk interior simulations. We also include non-zero stresses at the ISCO, which results in the disk effective temperature to increase rapidly towards the black hole, and give rise to rather extreme conditions with high temperatures and low surface densities. We found that the combined effects of torque at the inner edge and increased dissipation near the photosphere led to energetically significant hard spectral tails extending to beyond a hundred keV. We discuss the implications of our results in the context of the steep power law (SPL) state and the associated high-frequency quasi-periodic oscillations (HFQPO) observed in some X-ray binary systems. |
Saturday, April 13, 2019 3:54PM - 4:06PM |
D17.00003: Astrophysics with core-collapse supernova gravitational wave signals in the next generation of gravitational wave detectors Vincent J Roma, Jade Powell, Raymond Frey, Ik Siong Heng The next generation of gravitational wave detectors will improve the detection prospects for gravitational waves from core-collapse supernovae. The complex astrophysics involved in core-collapse supernovae pose a significant challenge to modeling such phenomena. The Supernova Model Evidence Extractor (SMEE) attempts to capture the main features of gravitational wave signals from core-collapse supernovae by using numerical relativity waveforms to create approximate models. These models can then be used to perform Bayesian model selection to determine if the targeted astrophysical feature is present in the gravitational wave signal. In this talk, I introduce SMEE and its recent extension to include g-modes and the standing accretion shock instability (SASI). I will discuss SMEE's performance for planned future detectors, such as the Einstein Telescope, Cosmic Explorer, and LIGO Voyager. |
Saturday, April 13, 2019 4:06PM - 4:18PM |
D17.00004: Extracting Physics from Gravitational Waves from Core-Collapse Supernovae Marek Szczepanczyk Core-Collapse Supernovae (CCSN) are spectacular and violent deaths of massive stars. The mechanism and properties of these explosions are not yet fully understood and observing gravitational waves (GW) from CCSN will provide some insight. In this talk, I will give an overview of GW searches targeting CCSN. I will present search results in the first two observing runs of Advanced LIGO and Virgo detectors. I will outline efforts towards GW parameter estimation and waveform reconstruction as well as prospects for detecting GW from CCSN with future GW detectors. |
Saturday, April 13, 2019 4:18PM - 4:30PM |
D17.00005: Exploring Core-Collapse Supernovae With Third-Generation Gravitational-Wave Detectors. Chaitanya Afle, Stefan W Ballmer, Duncan A. Brown, Adam Seth Burrows, David Radice, Varun Srivastava The observation of gravitational waves from core-collapse supernovae will |
Saturday, April 13, 2019 4:30PM - 4:42PM |
D17.00006: Initial data for general-relativistic simulations of generic black hole systems with electric charge, linear and angular momenta Gabriele Bozzola, Vasileios Paschalidis A quantity that has not received much attention in general-relativistic simulations of black holes is the electric charge. As a result, the dynamics of charged black holes in strong-field gravity and electromagnetism remains territory largely unexplored. One approach to tackling this problem is via the $3+1$ formulation of the coupled Einstein-Maxwell equations, where the spacetime and electromagnetic fields are found by evolving forward in time from an initial time slice. In this talk we present our work on generating valid initial data that describe $N$ black holes with electric charge, linear and angular momenta in the $3+1$ decomposition of spacetime. This is achieved by solving the Einstein and Maxwell constraint equations via the conformal transverse-traceless (Bowen-York) technique and treating the physical singularities as punctures. The electromagnetic fields are obtained from a superposition of boosted and rotated Kerr-Newman fields. Once the constraints are solved, we attribute the black hole physical parameters (mass, charge, and momenta) by applying the theory of dynamical horizons. Finally, we present our numerical implementation and results obtained for the case of two black holes. |
Saturday, April 13, 2019 4:42PM - 4:54PM |
D17.00007: Multi-mode black hole spectroscopy: detection and parameter estimation Vishal Baibhav, Emanuele Berti As current gravitational-wave detectors undergo technological improvements, we will soon reach an era when it would be possible to identify black hole merger remnants by measuring their quasinormal mode frequencies. This idea, often called “black hole spectroscopy”, is similar to identifying atomic elements through their spectral lines. I will address the question of event rates and detectability of quasinormal modes with current and planned detectors. I will show that while second-generation detectors are incapable of observing subdominant modes, space-based detector - like LISA - will see all harmonics currently available from numerical simulations. I will also explain how the detection of multiple ringdown modes can help in parameter estimation by breaking various degeneracies. This degeneracy breaking will be very important when detectors see only the ringdown (i.e., for intermediate-mass black hole mergers observed by ground-based detectors and for the heavier supermassive black hole mergers observed by LISA). |
Saturday, April 13, 2019 4:54PM - 5:06PM |
D17.00008: Numerical black hole binary mergers beyond general relativity Maria Okounkova, Mark A Scheel, Leo C Stein, Saul A Teukolsky At some scale, Einstein’s classical theory of general relativity (GR) must break and be reconciled with quantum mechanics in a beyond-GR theory. Binary black hole (BBH) mergers probe the non-linear, strong-field regime of gravity, and thus gravitational wave (GW) signals from these systems could contain signatures of a beyond-GR theory. However, numerical GW signal predictions have only been produced in GR, thus allowing for null and parametrized tests of GR, but no model-dependent test of gravity. I will present our recent work in producing numerical BBH waveforms in beyond-GR theories, starting with dynamical Chern-Simons gravity (DCS), an effective field theory with origins in string theory, loop quantum gravity, and inflation. In particular, I will present black hole gravitational waveforms from binary black hole collisions in DCS, analyze the quasi-normal mode spectra of the ringdown, and place detectability estimates on parameters governing this beyond-GR theory. Additionally, I will briefly discuss our recent work on numerical black hole shadows in DCS. |
Saturday, April 13, 2019 5:06PM - 5:18PM |
D17.00009: Frontiers at the interface of deep learning and large scale computing for Multi-Messenger Astrophysics Eliu Antonio Huerta We discuss recent developments at the interface of deep learning and large scale computing for the design and use of deep neural network models for the detection of gravitational waves in non-Gaussian and non-stationary noise, and the characterization of the binary components and the remnant of black hole mergers. We discuss the generality of these methodologies for the analysis of telescope image datasets, and showcase its application with the construction of large scale galaxy catalogs with the Dark Energy Survey. We also present neural network models, endowed with a statistical backbone, for gravitational wave parameter estimation analyses. |
Follow Us |
Engage
Become an APS Member |
My APS
Renew Membership |
Information for |
About APSThe American Physical Society (APS) is a non-profit membership organization working to advance the knowledge of physics. |
© 2021 American Physical Society
| All rights reserved | Terms of Use
| Contact Us
Headquarters
1 Physics Ellipse, College Park, MD 20740-3844
(301) 209-3200
Editorial Office
1 Research Road, Ridge, NY 11961-2701
(631) 591-4000
Office of Public Affairs
529 14th St NW, Suite 1050, Washington, D.C. 20045-2001
(202) 662-8700