Category: Uncategorized

Soham Bhattacharyya (Albert Einstein Institute, Max Planck Institute for Gravitational Physics)

Parameters extracted from Gravitational Wave (GW) data allow observers to quantify certain physical aspects of GW producing sources, like neutron stars (NS) and black holes (BH). In the case of an isolated BH, its physical shape in space, as a freely falling asymptotic observer would deduce from data, combined with its inertial mass, gets encoded in GWs radiated from these sources. In classical terms, a multipolar structure of radiating sources can be established from the GW data, giving a freely falling observer a dynamic view of the ‘horizon’ of a BH as it undergoes a damped oscillation towards a stable shape. However, the dynamical behavior is the opposite when the source is a binary system. Two ‘symmetric’ bodies mutually deform each other to a maximally distorted single compact object, radiating GWs that increase in frequency and amplitude (to specific maximum values) along with the distortion. Using a Zangenbewegung approach towards the maximal distortion (known in GW
 literature as the merger) from both sides (ring-down and inspiral, respectively), I will talk about GR’s predictions and the corresponding predictions made by extended theories of gravitation like f(R) and dynamical Chern-Simons.

Meeting ID:  854 3210 3337      Password: 959078

Anna Ijjas (Albert Einstein Institute, Max Planck Institute for Gravitational Physics)

I will discuss the detailed process by which slow contraction smooths and flattens the universe using an improved numerical relativity code that accepts initial conditions with non-perturbative deviations from homogeneity and isotropy along two independent spatial directions. Contrary to common descriptions of the early universe, I will show that the geometry first rapidly converges to an inhomogeneous, spatially-curved and anisotropic ultralocal state in which all spatial gradient contributions to the equations of motion decrease as an exponential in time to negligible values. This is followed by a second stage in which the geometry converges to a homogeneous, spatially flat and isotropic spacetime. In particular, the decay appears to follow the same history whether the entire spacetime or only parts of it are smoothed by the end of slow contraction.

Meeting ID:  854 3210 3337      Password: 959078

Andrew Chael (Princeton University)

Simulated images of a black hole surrounded by optically thin emission typically display two main features: acentral brightness depression and a narrow, bright “photon ring” consisting of strongly lensed images superposedon top of the direct emission. The photon ring closely tracks a theoretical curve on the image plane correspondingto light rays that asymptote to unstably bound photon orbits around the black hole. This critical curve has asize and shape that are purely governed by the Kerr geometry; in contrast, the size, shape, and depth of theobserved brightness depression all depend on the details of the emission region. For instance, images of sphericalaccretion models display a distinctive dark region—the “black hole shadow”—that completely fills the photonring. By contrast, in models of equatorial disks extending to the black hole’s event horizon, the darkest regionin the image is restricted to a much smaller area—aninner shadow—whose edge lies near the direct lensedimage of the equatorial horizon. Using both semi-analytic models and general relativistic magnetohydrodynamic(GRMHD) simulations, we demonstrate that the photon ring and inner shadow may be simultaneously visible insubmillimeter images of M87, where magnetically arrested disk (MAD) simulations predict that the emissionarises in a thin region near the equatorial plane. We show that the relative size, shape, and centroid of thephoton ring and inner shadow can be used to estimate the black hole mass and spin, breaking degeneracies inmeasurements of these quantities that rely on the photon ring alone. Both features may be accessible to directobservation via high-dynamic-range images with a next-generation Event Horizon Telescope.

Meeting ID:  854 3210 3337      Password: 959078

Francois Foucart (University of New Hampshire)

The first observation of a neutron star merger through gravitational waves and electromagnetic (EM) signals has shown us the power of multi-messenger observations. Multiple studies based on these observations have placed useful constraints on the equation of state of dense nuclear matter, while the event itself confirmed that mergers are likely (one of) the sources of r-process elements (e.g. gold, uranium) in the Universe. Many interpretations of these observations require reliable models for kilonovae, the radioactively powered EM transient powered by mergers. The numerical simulations that typically inform kilonovae models however have two important “known unknowns’’, namely the uncertainties due to approximate modeling of magnetic fields and neutrinos. In this talk, I will review the role of neutrinos in neutron star-neutron star mergers, as well as existing approximate transport methods used in simulations. I will also present a Monte-Carlo algorithm recently implemented in the SpEC code, used to perform the first simulations of merging neutron stars that directly attempt to solve Boltzmann’s equation of radiation transport. This scheme is purposely built to be as inexpensive as possible: the cost of a simulation remains comparable to simulations using our best existing approximate transport scheme. I will discuss the trade-offs made to reach that target, and how the scheme may be improved in the future. Related papers: arXiv:2103.16588, arXiv:2008.08089

Meeting ID:  854 3210 3337      Password: 959078

José A. Pons

It is generally accepted that the nonlinear, dynamical evolution of magnetic fields in the interior of neutron stars plays a key role in the explanation of the observed phenomenology (temperatures, luminosities, spin period and derivative). Understanding the transfer of energy between toroidal and poloidal components, or between different scales, is of particular relevance. In this talk I discuss the general aspects of the long term magnetic and thermal evolution, with particular emphasis in the role of the Hall drift and ambipolar diffusion for typical magnetar conditions

Meeting ID:  854 3210 3337        Password: 959078

David Julián Mateos Solé (Universitat de Barcelona)

Cosmological phase transitions proceed via the nucleation of bubbles that subsequently expand and collide. The resulting gravitational wave spectrum depends crucially on the bubble wall velocity. Microscopic calculations of this velocity are challenging even in weakly coupled theories. I will show how to use holography to compute the wall velocity from first principles in strongly coupled, non-Abelian, four-dimensional gauge theories. No previous knowledge of holography or string theory required.

Meeting ID:  854 3210 3337        Password: 959078

Jan Röder (Institut für Theoretische Physik, Goethe -Universität Frankfurt)

Boris Daszuta (Friedrich-Schiller-Universität Jena)

`GR-Athena++` is a general-relativistic, high-order, vertex-centered solver that extends the oct-tree, adaptive mesh refinement capabilities of the astrophysical (radiation) magnetohydrodynamics code `Athena++`. To simulate dynamical spacetimes `GR-Athena++` uses the Z4c evolution scheme of numerical relativity coupled to the moving puncture gauge. Stable and accurate binary black hole merger evolutions are demonstrated in convergence testing, cross-code validation, and verification against state-of-the-art effective-one-body waveforms. `GR-Athena++` leverages the task-based parallelism paradigm of `Athena++` to achieve excellent scalability. Strong scaling efficiencies above 95% for up to 1.2×1e4 CPUs and excellent weak scaling up to 1e5 CPUs in a production binary black hole setup with adaptive mesh refinement are measured. `GR-Athena++` thus allows for the robust simulation of compact binary coalescences and and offers a viable path towards numerical relativity at exascale.

Zoom Meeting ID: 854 3210 3337
Passcode: 959078