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:20260627T142746Z UID:e87748f4-f527-44f0-b407-f89959e27d79 SEQUENCE:1 CREATED:20251027T150912Z DESCRIPTION: Compact binaries with asymmetric mass ratios are key expected sources for next-generation gravitational-wave detectors. Gravitational s elf-force theory has been successful in producing post-adiabatic waveforms that describe the quasicircular inspiral around a nonspinning black hole with sub-radian accuracy\, in remarkable agreement with numerical relativi ty simulations. These models are based on a two-stage process\, which make s 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 innerm ost stable circular orbit (ISCO)\, missing the final merger and ringdown s tages. In this talk\, I will show how the inspiral’s “phase-space” a pproach can be extended beyond the ISCO\, building first-principles inspir al-merger-ringdown waveforms within self-force theory\, and I will compare these waveforms with a self-consistently calculated sum over quasinormal modes at late times. Finally\, I will briefly discuss how beyond-GR effect s can be modularly added in this framework. Based on arXiv:2405.00170\, 25 06.02189 and 2510.11793. LAST-MODIFIED:20251027T150912Z LOCATION:DF Seminar Room (2-8.3)\, 2nd floor of Physics Building URL:http://df.vps.tecnico.ulisboa.pt/en/events/inspiral-merger-ringdown-wa veforms-from-gravitational-self-force-theory/ X-ALT-DESC;FMTTYPE=text/html:

Compact binaries w ith asymmetric mass ratios are key expected sources for next-generation gr avitational-wave detectors. Gravitational self-force theory has been succe ssful in producing post-adiabatic waveforms that describe the quasicircula r inspiral around a nonspinning black hole with sub-radian accuracy\, in r emarkable 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- computed as functions on the orbital phase space\; in a (fast) online stag e\, the waveform is generated by evolving through the phase space.
Current inspiral models\, however\, break down at the innermost stable circular orbit (ISCO)\, missing the final merger and ringdown stages. In t his talk\, I will show how the inspiral’s “phase-space” approach can be extended beyond the ISCO\, building first-principles inspiral-merger-r ingdown waveforms within self-force theory\, and I will compare these wave forms with a self-consistently calculated sum over quasinormal modes at la te times. Finally\, I will briefly discuss how beyond-GR effects can be mo dularly added in this framework. Based on arXiv:2405.00170\, 2506.02189 an d 2510.11793.

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