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 H08: Gravitational Waveform Modeling |
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Sponsoring Units: DGRAV Chair: Maya Fishbach, Canadian Institute for Theoretical Astrophysics Room: Symphony III - 2nd Floor |
Sunday, April 16, 2023 1:30PM - 1:42PM |
H08.00001: Waveform accuracy and systematic uncertainties in current gravitational wave observations Caroline B Owen, Carl-Johan O Haster, Scott E Perkins, Neil J Cornish, Nicolas Yunes The post-Newtonian formalism plays an integral role in the models used to extract information from gravitational wave data, but models that incorporate this formalism are inherently approximations. Disagreement between an approximate model and nature will produce mismodeling biases in the parameters inferred from data, introducing systematic error. Through an injection and recovery campaign, we undertake a proof-of-principle study of such systematic error. In particular, we study how unknown, but calibrated, higher-order post-Newtonian corrections to the gravitational wave phase impact systematic error in recovered parameters. We consider injected data of non-spinning binaries as detected by a current, second-generation network of ground-based observatories and recover them with models of varying PN order in the phase. We will show that the truncation of higher order (>3.5) post-Newtonian corrections to the phase can produce significant systematic error even at signal-to-noise ratios of current detector networks. Additionally, we will present a method to mitigate systematic error by marginalizing over our ignorance in the waveform through the inclusion of higher-order post-Newtonian coefficients as new model parameters and show that this method can reduce systematic error greatly at the cost of increasing statistical error. |
Sunday, April 16, 2023 1:42PM - 1:54PM |
H08.00002: Up-down binaries are unstable and we want to know Viola De Renzis, Davide Gerosa
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Sunday, April 16, 2023 1:54PM - 2:06PM |
H08.00003: Time- and frequency-domain waveform models for the gravitational-wave memory effect Arwa Z Elhashash, David A Nichols After the passage of a gravitational-wave (GW) signal, a permanent relative displacement between two freely falling test masses generically occurs, which is called the GW memory effect. Searches for the memory effect in GW detector data require accurate waveform models, which must be evaluated many times (and, thus, need to be evaluated rapidly). Current analytical waveform models and many numerical-relativity waveforms and surrogates of binary-black-hole (BBH) mergers do not include the memory effect. Instead, GW memory is computed from waveforms without memory by using conservation laws in asymptotically flat spacetimes, which is relatively slow. We therefore develop time- and frequency-domain waveform models of the GW memory effect for nonspinning BBH mergers for comparable-mass systems. We also develop a fit for the final memory offset that incorporates data from both comparable and extreme mass-ratio limits. In addition to speeding up GW searches, having these analytic models will give analytical insight into the time- and frequency-domain properties of the GW memory signal. |
Sunday, April 16, 2023 2:06PM - 2:18PM |
H08.00004: Gravitational-wave signatures of dark-matter capture in intermediate mass-ratio inspirals David A Nichols When particle dark matter (DM) is bound gravitationally around a massive black hole (BH) in sufficiently high densities, the DM will affect the rate of inspiral of a secondary compact object that forms a binary with the massive BH. For intermediate mass-ratio inspirals (IMRIs), the dominant difference from inspirals in vaccum arises from dynamical friction acting on the secondary. However, if the secondary is a stellar-mass BH, then it can capture some of the DM as it inspirals in the DM distribution and increase in mass. Prior work (assuming a static DM distrubtion during the inspiral) showed that DM capture has a subdominant effect compared to that of dynamical friction, but it can still be large enough to cause substantial dephasing of these systems from those in vacuum and those with DM where the effect of just dynamical friction was modeled. In this talk, I will revisit these prior estimates of the impact of DM capture on the emitted gravitational waves from IMRIs of binary BHs. I will show there is a region of parameter space of binaries for which estimates of the capture were too large (specifically, because the DM distribution was assumed to be unchanging throughout the inspiral, thereby allowing the secondary BH to capture more mass in DM than that enclosed within the orbit of the secondary). To restore consistency in these scenarios, I will discuss a method to evolve the DM distribution such that the mass captured by the secondary never exceeds the enclosed mass. |
Sunday, April 16, 2023 2:18PM - 2:30PM |
H08.00005: Persistent Gravitational Wave Observables from Post-Newtonian Compact Binaries. Siddhant Siddhant, David A Nichols, Alexander M Grant Persistent gravitational wave (GW) observables are generalizations of the GW memory effect that contain time-integrated changes in the spacetime curvature between two non-radiative regions. In asymptotically flat space-times at leading order in luminosity distance, these observables are determined by different temporal moments of the time derivative of the GW strain (the news tensor). These moments arise predominantly from nonlinear terms in the Einstein equations that can be challenging to evaluate numerically or with high-order analytical calculations; however, they can be inferred from lower-order waveforms for which the moments vanish by sequentially integrating the Bondi-Sachs evolution and conservation equations. We use these equations to calculate the leading post-Newtonian (PN) contributions to the moments of the news for compact-binary sources. While these moments are measurable by observers in relative acceleration far from an isolated source, they are not easily accessible to current interferometric GW detectors, such as LIGO, which are calibrated to measure the GW strain. We therefore identify components of the GW strain that are responsible for these moments. We find that the PN order of these moments increases for higher-order moments of the news. |
Sunday, April 16, 2023 2:30PM - 2:42PM |
H08.00006: Evolving intermediate-mass-ratio inspirals in the presence of dark matter Benjamin Wade, David A Nichols, Alexander M Grant Intermediate mass black holes (IMBHs) can grow in dark matter environments and form locally dense distributions of dark matter called mini-spikes. We consider the environmental effects of such a spike on the inspiral of a stellar mass compact object into an IMBH. Previous studies demonstrated that dynamical friction acting from the dark matter on the inspiraling compact object has measurable effects in the emitted gravitational waves from the system, which the LISA mission could measure. However, these studies made several simplifying assumptions both in how the dark matter was evolved and in how the dynamical friction was computed. In this talk, I will discuss progress in evolving the dark matter distribution function through the collisionless Boltzmann equation and in computing the dynamical friction through resonant torques. Using these methods, we can more accurately determine the gravitational waveform from these systems. |
Sunday, April 16, 2023 2:42PM - 2:54PM |
H08.00007: A Hybridized Surrogate Model using CCE Waveforms Jooheon Yoo, Keefe Mitman, Vijay Varma With recent improvements in the Cauchy-characteristic evolution (CCE) procedure, CCE waveforms could become the new standard method of extracting gravitational waveforms at $mathcal{I}^+$ from numerical relativity simulations. Unlike the waveforms extracted using the extrapolation method, CCE waveforms capture memory effects expected to be observed using next-generation detectors. We present a new surrogate model built with CCE waveforms, NRSur3dq8\_CCE. This model is trained over the same 3-dimensional parameter space as the previous model NRSur3dq8, but now using CCE waveforms: $q leq 8 ext{ and } vertchi_{1z}vert,~ vertchi_{2z}vert leq 0.8$ |
Sunday, April 16, 2023 2:54PM - 3:06PM |
H08.00008: Optimizing post-Newtonian parameters and fixing the BMS frame for numerical relativity waveform hybridizations Dongze Sun, Michael Boyle, Keefe Mitman, Mark A Scheel, Leo C Stein, Saul A Teukolsky, Vijay Varma Numerical relativity (NR) simulations of binary black holes (BBH) provide precise waveforms, but are typically too computationally expensive to produce waveforms long enough to cover the whole frequency band of gravitational wave observatories. Consequently, it is important to be able to hybridize NR waveforms with analytic, post-Newtonian (PN) waveforms. We show that to build such hybrids, it is important to both optimize over the PN parameters as well as fix the Bondi-van~der~Burg-Metzner-Sachs (BMS) frame of the NR waveforms to match that of PN theory. With this procedure, we find that for spin-aligned systems, we can reduce the typical mismatches between NR and PN over 20-orbit-long waveforms to the error caused by non-zero eccentricities of NR systems, which is around e2 ~10-7. And for precessing systems, we can obtain typical mismatches of 10-5, which are limited by the truncation of spin-asymmetric memory terms in PN waveforms at 2PN order. |
Sunday, April 16, 2023 3:06PM - 3:18PM |
H08.00009: Analytic multi-messenger signals from magnetized compact binary mergers Maria C Hamilton, Alexander O'Dell The simultaneous detection of both gravitational waves (GWs) and a short-duration gamma-ray burst (GRB) coined as GW170817/GRB 170817A, started the new field of Multi-Messenger Gravitational Wave Astronomy. Although magnetized compact binary mergers are widely accepted as sources of GRBs, the mechanism behind jet formation is still unsettled. We report on a novel implementation of fully analytical GW templates and electromagnetic (EM) radiation amplification during the merger of binary black holes (BBH) and binary neutron stars (BNS) using Python within the Jupyter Notebook. We start with a BBH system and calculate the GWs using the post-Newtonian (PN) formalism for the inspiral evolution and the Backwards-one-Body (BoB) model for the merger. We overlap the signal at the light ring (LR) and test our hybrid waveform against numerical relativity (NR) simulations. We add the magnetic field and investigate the EM amplification by calculating the evolution of the Poynting luminosity during merger. We introduce next tidal effects to account for the coupling between matter and spacetime, present during the merger of a BNS system, and compare again our GW template with NR predictions. Lastly, we repeat the Poynting luminosity calculation, to analyze how the addition of matter changes the magnetic field amplification driven by the highly dynamical, strong gravitational field during the merger. Our results are relevant for the characterization of compact binary mergers accompanied by EM counterparts. |
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