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 V15: Mini-symposium: Multimessenger Astrophysics and Nuclear Physics IIMini-Symposium
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Sponsoring Units: DNP DGRAV Chair: Saul Beceiro Novo, Universidade da Coruña Room: Marquette VI - 2nd Floor |
Tuesday, April 18, 2023 3:45PM - 3:57PM |
V15.00001: Needle in a Bayes Stack: a Hierarchical Bayesian Method for Constraining the Neutron Star Equation of State with an Ensemble of Binary Neutron Star Post-merger Remnants Alexander W Criswell, Jesse Miller, Noah Woldemarium, Theodoros Soultanis, Andreas Bauswein, Katerina Chatziioannou, Michael W Coughlin, Galin Jones, Vuk Mandic Binary neutron star (BNS) post-merger gravitational-wave emission occurs in the aftermath of a BNS merger as an unstable hypermassive remnant experiences quadrupolar oscillations and non-axisymmetric deformations. The post-merger gravitational-wave spectrum possesses a characteristic peak frequency that has been shown to be dependent on the binary chirp mass and the neutron star equation of state (EoS), rendering post-merger gravitational waves a powerful tool for constraining neutron star composition. Unfortunately, the BNS post-merger signal is unlikely to be detected with sufficient signal-to-noise ratio (SNR) for this purpose until the advent of next-generation detectors. However, by employing empirical relations derived from numerical relativity simulations, we can combine information across an ensemble of BNS mergers, allowing us to obtain EoS constraints in the low-SNR limit. We present a hierarchical Bayesian method for deriving constraints on the neutron star EoS through an ensemble analysis of binary neutron star mergers and discuss the prospects of our analysis as applied to realistic simulations of BNS observations with current-generation gravitational wave detectors. |
Tuesday, April 18, 2023 3:57PM - 4:09PM |
V15.00002: A detailed study of the impact of mass ejecta and velocity profiles on kilonova properties with GEMMA Amelia M Henkel, Francois V Foucart, Geert Raaijmakers, Samaya M Nissanke The first observation of a binary neutron star merger GW170817/AT2017gfo ushered the world into a new era of multimessenger astronomy. The event elucidated many then-unknown properties of neutron star mergers, such as their nucleosynthetic yields and many aspects of their merger dynamics. However, many features of GW170817/AT2017gfo and binary neutron star mergers in general remain uncertain, including detailed information about the mass ejection processes. GEMMA is a state-of-the-art multimessenger analysis tool whose primary function is to provide forward and backward modeling of binary neutron star and neutron star-black hole mergers. Here, we expand upon GEMMA’s capabilities to accept a series of formulae derived from numerical relativity simulations for binary neutron star mass ejection and velocity profiles. We assume a two-component ejecta model consisting of dynamical ejecta and post-merger disk ejecta, which each have distinct observable properties. We then compare the relative performance of the ejecta models to each other and to AT2017gfo to identify predominant sources of uncertainty in kilonova lightcurves. We also vary intrinsic binary parameters, such as the mass ratio and tidal deformability, to ascertain their influence on the resultant lightcurves. |
Tuesday, April 18, 2023 4:09PM - 4:21PM Withdrawn |
V15.00003: Probing AGN as Astrophysical Neutrino Sources with Millimeter-Wavelength Activity Alina L Kochocki In the past ten years, the IceCube South Pole Neutrino Observatory has revealed a neutrino sky in conflict with previous expectations from theory and multi-wavelength observations. While a diffuse flux of astrophysical neutrinos has been well established, certain analyses have found difficulty reconciling this intensity with expected neutrino source classes. Additionally, the discovery of the high-energy, transient neutrino source, TXS 0506+056, has drawn further attention to blazars, and the association of their activity with gamma-ray emission. More recently, the opacity of such environments to high-energy photons has been highlighted. Here, we discuss millimeter-wavelength observations of variable AGN as a robust tracer for neutrino activity. The relation of synchrotron emission at this wavelength to neutrino production is explored, and a first correlation of IceCube data with millimeter light curves from the Atacama Cosmology Telescope is discussed. |
Tuesday, April 18, 2023 4:21PM - 4:33PM |
V15.00004: Equations of State at Finite Temperature And Out of Equilibrium Calibrated Using Chiral Effective Field Theory Liam Brodie, Mark Alford, Alexander Haber, Ingo Tews The equation of state (EoS) for nuclear matter at finite temperature and out of equilibrium is a fundamental ingredient for simulations of binary neutron star mergers, calculation of cooling curves, and other transport properties. We construct four new EoSs using a relativistic mean-field theory (RMF). Typically, the couplings in an RMF are fit to isospin-symmetric nuclear matter data, but the matter in isolated neutron stars is much closer in composition to pure neutron matter. In this work, along with reproducing isospin-symmetric nuclear matter data, we also fit our RMF to pure neutron matter calculations from chiral effective field theory. These calculations are needed because it is not possible to perform experiments on pure neutron matter on Earth. Our EoSs agree with current mass and radius measurements from NICER and LIGO. |
Tuesday, April 18, 2023 4:33PM - 4:45PM |
V15.00005: Bulk Visocisty in Neutron Star Merger Ziyuan Zhang, Mark Alford Transport phenomena plays an important role in neutron star merger. Bulk viscosity is a resonance transport phenomena arising from the competition between the density oscillation and the weak interaction equilibration. We calculate bulk viscosity in the neutrino-transparent regime of nuclear matter and find it to be important for the merger simulation. |
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