Registration Room: Physics Department - Aula Amaldi (Marconi Building)

Welcome from SOC and from INFN Roma1 Director Room: Physics Department - Aula Amaldi (Marconi Building)

TEONGRAV: an INFN initiative for the Theory of Gravitational Wave Sources

• Bruno Giacomazzo (Milano-Bicocca)

Room: Physics Department - Aula Amaldi (Marconi Building)

Beyond the horizon: The status and future of gravitational-wave source modelling in general relativity

• Geraint Pratten (University of Birmingham)

Room: Physics Department - Aula Amaldi (Marconi Building) This is an overview talk that will outline the progress that has been made in modelling the gravitational-wave signal emitted by coalescing compact binaries. I will briefly introduce the key paradigms and modelling techniques that have led to the successful construction of numerous waveform models before discussing some of the challenges that we face as we transition to the next generation of gravitational wave detectors. Where possible, I will highlight new avenues of exploration that are yielding novel insights into the behaviour of compact binaries in the strong-field regime.

Eleonora Troja Room: Physics Department - Aula Amaldi (Marconi Building) TBA

Numerical Relativity for strong field tests of gravity.

• Helvi Witek (University of Illinois Urbana-Champaign (UIUC))

Room: Physics Department - Aula Amaldi (Marconi Building) TBA

Waveform modelling for extreme and intermediate mass-ratio inspirals using a multi-scale self-force approach

• Niels Warburton (UCD)

Room: Physics Department - Aula Amaldi (Marconi Building) The calculation of gravitational wave templates for binaries with disparate masses can be achieved using a (small mass ratio) perturbative expansion. This “self-force” approach was recently pushed to second-order (in the mass ratio) which has enabled the modelling of a wide class of binaries with mass ratios ranging ~10^5:1 to ~30:1. Furthermore, by employing a multi-scale expansion the associated gravitational waveforms can be directly computed on sub-second timescales without the need for any further waveform acceleration. In this talk I will review the multi-scale self-force approach and outline the ongoing program to extend current calculations to cover the full precessing and eccentric parameter space

Modeling and observational status of black hole vibrational spectra

• Gregorio Carullo

Room: Physics Department - Aula Amaldi (Marconi Building) Dark compact objects are nowadays routinely observed through multiple experimental schemes. Measurements of their vibrational spectra offer unprecedented opportunities to investigate the highly dynamical regime of General Relativity, search for signs of new physics, and increase the evidence for their "black hole nature". After an introduction to the topic, I will review recent achievements of this scientific program enabled by gravitational-wave observations, and current efforts to extend it through the inclusion of nonlinear effects and generic orbital configurations of binary mergers. Prospects for high-precision measurements through next-generation interferometric detectors will also be discussed, together with their potential to address many open questions in fundamental physics.

The origin and growth of supermassive black holes

• Raffaella Schneider (Sapienza University, INFN)

Room: Physics Department - Aula Amaldi (Marconi Building)

TEONGRAV Members Meeting Room: Physics Department - Aula Amaldi (Marconi Building)

Probing ultra-dense matter with gravitational waves

• Micaela Ortel

Room: Physics Department - Aula Amaldi (Marconi Building) The first detection of gravitational waves from a merging neutron star binary system and the accompanying observations of electromagnetic counterparts in 2017 demonstrated the enormous potential of multi-messenger astronomy for understanding the properties of ultra-dense matter. Neutron stars --relict of the gravitational collapse and subsequent supernova explosion of a massive star at the end of his life-- comprise the highest densities of matter that can stably exist in the Universe. During this talk, I will discuss the possibilities for insights on matter under these extreme conditions from future detections of the gravitational wave signals emitted from events involving neutron stars. In particular, results will be shown illustrating the capacity of multi-messenger observations to give us hints about a possible phase transition in neutron star matter.

Astrophysics with BH mergers: making sense of a jumble of everything

• Martyna Chruślińska (Max Planck Institute for Astrophysics)

Room: Physics Department - Aula Amaldi (Marconi Building) The rate of GW detections will soar from hundreds to millions per year as detectors improve, revealing the population properties of BH mergers in great detail. Such properties encode valuable information about how stars form and evolve in galaxies very different from our own. They can provide complementary constraints on the cosmic chemical history and on star formation in environments that evade electromagnetic observations. However, the use of GWs in astrophysics presents challenges that must be overcome to realise their full potential. In particular, the astrophysical "interpretation challenge" that I will discuss in my talk. The observable BH merger population contains a mixture of systems formed throughout the Universe, with different chemical compositions and in very different environments (allowing for unique formation channels). Both strongly influence the formation of BH mergers and can degenerate into their population properties. One aspect that is key to breaking such degeneracies, and which I will focus on, is constraining the iron-dependent cosmic star formation history.

Neutron star equation of state measurements from binary mergers

• Rossella Gamba (Pennsylvania State University / University of California, Berkeley)

Room: Physics Department - Aula Amaldi (Marconi Building) The study of neutron stars, dense remnants of stellar core collapse, provides a unique opportunity to explore the fundamental properties of matter under extreme conditions. In this talk I will review the status of our current understanding of the neutron star equation of state (EOS) through measurements derived from multi-messenger observations of binary neutron star mergers. Then, focusing on the inspiral-to-post-merger gravitational wave emission, I will discuss the prospect of constraining the EOS with third generation detectors such as Einstein Telescope and Cosmic Explorer, pointing out their potential as well as the challenges that their increased sensitivity will pose.

Electromagnetic signatures from GW events

• Daniel Siegel (University of Greifswald, Germany)

Room: Physics Department - Aula Amaldi (Marconi Building)

Final remarks and good byes Room: Physics Department - Aula Amaldi (Marconi Building)