BEGIN:VCALENDAR VERSION:2.0 PRODID:-//linuxsoftware.nz//NONSGML Joyous v1.4//EN BEGIN:VEVENT SUMMARY:Inspiral-merger-ringdown waveforms from gravitational self-force t heory DTSTART:20251030T143000Z DTEND:20251030T160000Z DTSTAMP:20260617T192222Z UID:e87748f4-f527-44f0-b407-f89959e27d79 SEQUENCE:2 CREATED:20251027T150922Z DESCRIPTION:Compact binaries with asymmetric mass ratios are key expected sources for next-generation gravitational-wave detectors. Gravitational se lf-force theory has been successful in producing post-adiabatic waveforms that describe the quasicircular inspiral around a nonspinning black hole w ith sub-radian accuracy\, in remarkable agreement with numerical relativit y simulations. These models are based on a two-stage process\, which makes waveform generation very efficient: in a (slow) offline stage\, waveform ingredients are pre-computed as functions on the orbital phase space\; in a (fast) online stage\, the waveform is generated by evolving through the phase space. Current inspiral models\, however\, break down at the innermo st stable circular orbit (ISCO)\, missing the final merger and ringdown st ages. In this talk\, I will show how the inspiral’s “phase-space” ap proach can be extended beyond the ISCO\, building first-principles inspira l-merger-ringdown waveforms within self-force theory\, and I will compare these waveforms with a self-consistently calculated sum over quasinormal m odes at late times. Finally\, I will briefly discuss how beyond-GR effects can be modularly added in this framework. Based on arXiv:2405.00170\, 250 6.02189 and 2510.11793. LAST-MODIFIED:20251027T150933Z LOCATION:DF Seminar Room (2-8.3)\, 2nd floor of Physics Building URL:http://df.vps.tecnico.ulisboa.pt/pt/eventos/inspiral-merger-ringdown-w aveforms-from-gravitational-self-force-theory/ X-ALT-DESC;FMTTYPE=text/html:

Compact binaries wi th asymmetric mass ratios are key expected sources for next-generation gra vitational-wave detectors. Gravitational self-force theory has been succes sful in producing post-adiabatic waveforms that describe the quasicircular inspiral around a nonspinning black hole with sub-radian accuracy\, in re markable agreement with numerical relativity simulations.

These models are based on a two-stage process\, which makes waveform generation very efficient: in a (slow) offline stage\, waveform ingredients are pre-c omputed as functions on the orbital phase space\; in a (fast) online stage \, the waveform is generated by evolving through the phase space.

Current inspiral models\, however\, break down at the innermost stable c ircular orbit (ISCO)\, missing the final merger and ringdown stages. In th is talk\, I will show how the inspiral’s “phase-space” approach can be extended beyond the ISCO\, building first-principles inspiral-merger-ri ngdown waveforms within self-force theory\, and I will compare these wavef orms with a self-consistently calculated sum over quasinormal modes at lat e times. Finally\, I will briefly discuss how beyond-GR effects can be mod ularly added in this framework. Based on arXiv:2405.00170\, 2506.02189 and 2510.11793.

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