Bulletin of the American Physical Society
APS April Meeting 2023
Volume 68, Number 6
Minneapolis, Minnesota (Apr 15-18)
Virtual (Apr 24-26); Time Zone: Central Time
Session D14: Gravitational-Wave Astronomy |
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Sponsoring Units: DAP Chair: David Wright, University of Central Florida Room: Marquette V - 2nd Floor |
Saturday, April 15, 2023 3:45PM - 3:57PM |
D14.00001: Low-frequency Gravitational Waves from Massive Black Hole Binaries Luke Z Kelley The NANOGrav Pulsar Timing Array (PTA) detected a low-frequency (nanohertz) common process in our 12.5yr data that is consistent with expectations for a stochastic gravitational wave (GW) background. Such a background has long been predicted from the ensemble of millions of massive black hole (MBH) binaries distributed throughout the Universe. Our upcoming 15yr dataset provides far more leverage on the nature of this signal, allowing for unprecedented constraints on its possible origin. In this talk, I will discuss the wealth of information encoded within this GW cacophony, highlighting our group's new simulation frameworks to comprehensively model MBH populations and make astrophysical constraints. I will also present future prospects for complementing GW measurements from PTAs with electromagnetic counterparts from surveys of active galactic nuclei, and the unique insights that these low-frequency multi-messenger signals will unveil in the coming years. In addition to its own significant breakthroughs, I will mention how the nanohertz regime serves as a crucial testbed for the LISA mission, which will transform our understanding of MBHs both nearby and out to the early Universe.
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Saturday, April 15, 2023 3:57PM - 4:09PM |
D14.00002: Future Prospects for Spectral Characterisation of the Gravitational Wave Background with Pulsar Timing Arrays William Lamb, Stephen R Taylor, Xavier Siemens Pulsar Timing Arrays may soon detect a nanohertz-frequency gravitational wave background, which is likely dominated by gravitational waves from a population of supermassive black holes binaries. However, the spectrum of the background may encode the dynamics and demographics of the binary population, as well as sub-dominant signatures of gravitational waves from the early universe. In this talk, we present studies of parameter estimation and model selection of the gravitational-wave background over numbers of pulsar and frequencies using rapid and accurate refitting techniques, and show initial investigations into distinguishing a cosmological signal from an astrophysical background. |
Saturday, April 15, 2023 4:09PM - 4:21PM |
D14.00003: Characterizing LISA-band gravitational-wave signals from eccentric compact binaries orbiting a supermassive black hole Alan M Knee, Jessica McIver, Smadar Naoz, Bao-Minh Hoang, Isobel M Romero-Shaw Compact binaries situated in galactic nuclei may be gravitationally perturbed by the central supermassive black hole (SMBH) of the host galaxy. The interaction between the inner compact binary and the outer SMBH can induce eccentricity oscillations in the former through the eccentric Kozai-Lidov mechanism. During periods of high eccentricity, these binaries emit a broadband gravitational-wave (GW) spectrum detectable by LISA, with signal-to-noise ratios potentially in excess of 100. The time-domain GW signal from these systems consists of a series of repeated bursts associated with individual periastron passages, with additional amplitude modulations due to SMBH-induced changes in the orientation of the inner binary. We present preliminary results from a study aimed at characterizing these repeating signals after propagating them through to the LISA time-delay interferometry strain channels. We further explore search methods for identifying these systems in the presence of other astrophysical GW sources and non-astrophysical glitches included in the Spritz edition of the LISA data challenges. |
Saturday, April 15, 2023 4:21PM - 4:33PM |
D14.00004: Multimessenger Cocoons in Dying Stars: New LIGO-Detectable Gravitational Wave Sources Ore Gottlieb, Hiroki Nagakura, Alexander Tchekhovskoy, Priyamvada Natarajan, Enrico Ramirez-Ruiz, Jonatan Jacquemin-Ide, Nick Kaaz, Vicky Kalogera Upcoming LIGO/Virgo/KAGRA (LVK) observing runs promise to detect a variety of inspiralling gravitational wave (GW) sources. With powerful phenomena such as gamma-ray bursts and supernovae unable to produce detectable GW signals in LVK, all non-inspiral GW sources remain firmly out of reach for the next decade. Using state-of-the-art simulations that for the first time, follow jets from a newly formed black hole (BH) in a collapsing star to outside the star, I will present the first class of non-inspiral GW sources, that is powerful and abundant enough such that its detection by LVK can be imminent. The BH-powered jets wobble inside the star and inflate an energetic bubble - cocoon, which inevitably develop turbulence with a broad power spectrum that translates into broadband, powerful quasi-isotropic GW emission within the LVK band. The GW emission is well within our observational grasp as the estimated detection rate is 0.1--3 events in LVK runs O3/O4. With a detection horizon of ~100 Mpc, these GWs are expected to be accompanied by detectable energetic core-collapse supernova and cocoon electromagnetic emission, making jetted stellar explosions promising multi-messenger sources, enabling targeted searches for GWs based on the electromagnetic counterpart detection. |
Saturday, April 15, 2023 4:33PM - 4:45PM |
D14.00005: Dropping Anchor: Understanding the Populations of Binary Black Holes with Random and Aligned Spin Orientations Vishal Baibhav, Zoheyr Doctor, Vicky Kalogera The relative spin orientations of black holes (BHs) in binaries encode their evolutionary history: BHs assembled dynamically should have isotropically distributed spins, while spins of the BHs originating in the field should be aligned with the orbital angular momentum. |
Saturday, April 15, 2023 4:45PM - 4:57PM |
D14.00006: Subtracting Compact Binary Foregrounds to Search for Subdominant Gravitational-Wave Backgrounds in Next-Generation Ground-Based Observatories Bei Zhou, Luca Reali, Emanuele Berti, Mesut Çaliskan, Cyril Creque-Sarbinowski, Marc P Kamionkowski, Bangalore S Sathyaprakash
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Saturday, April 15, 2023 4:57PM - 5:09PM |
D14.00007: The landscape of stellar mass black hole spectroscopy with the Einstein Telescope and Cosmic Explorer Costantino Pacilio Black hole spectroscopy is the measurement of the quasi normal mode spectrum in the gravitational waves emitted by a remnant black hole from a binary merger. Detecting multiple excited modes provides an excellent opportunity to test the dynamics of general relativity in the strong field regime and the hypothesis that the final object relaxes to a Kerr black hole. Third generation detectors will be a quantum leap for black hole spectroscopy thanks to a large increase in the ringdown signal-to-noise ratio (SNR), which will allow to identify routinely subdominant excited modes besides the dominant one. We use a simulated catalog of merging stellar mass binary black holes to investigate the prospects of black hole spectroscopy with ground based third generation detectors, with particular emphasis on the Einstein Telescope working in synergy with a Cosmic Explorer detector. We study the cumulative distribution in the ringdown SNR and quantify the precision with which the quasi normal modes will be measured during the operational time of the detectors. Overall, we find that third generation detectors will allow to detect several thousands of ringdown events per year, with O(10) golden events per year with SNR larger than 100. Next, we find that about a thousand events per year will alow to constrain deviations from general relativity in the spectrum with better than 10 per cent precision in the individual events. Finally, we discuss the prospects for constraining deviations from general relativity when stacking together the population of the detected events. |
Saturday, April 15, 2023 5:09PM - 5:21PM |
D14.00008: Effect of magnetization at late times on PPI-saturated self-gravitating accretion disks: simulations in full GR Erik K Wessel, Vasileios Paschalidis, Antonios Tsokaros, Milton Ruiz, Stuart L Shapiro We present the results of our dynamical-spacetime magnetohydrodynamic study on the effects of magnetic fields on self-gravitating accretion disks around spinning black holes (a/M = 0.7). When no magnetic fields are present, these systems are unstable to the Papaloizou-Pringle Instability (PPI) which saturates and produces strong gravitational waves (GW), detectable to cosmological distances by third-generation GW observatories. Prior studies in fixed spacetime have shown that small seed fields can initiate rapid growth of the magneto-rotational instability (MRI) in disks without self-gravity, which strongly suppresses the PPI and prevents GW emission. Here we instead wait for the self-gravitating disks to reach a PPI-saturated state, then insert small seed magnetic fields to test how they could effect the dynamics of highly asymmetric massive disks. For spinning and non-spinning black holes, we find the MRI reduces the amplitude of PPI modes and their associated GWs. Magnetic fields reduce the maximum detection distance by Cosmic Explorer from 300 Mpc to 45 Mpc for a 10 solar mass system, by LISA from 11500 Mpc to 2700 Mpc for a 2 × 105 solar mass system, and by DECIGO from z ≈ 5 down to z ≈ 2 for a 1000 solar mass system. |
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