BEGIN:VCALENDAR VERSION:2.0 PRODID:-//linuxsoftware.nz//NONSGML Joyous v1.4//EN BEGIN:VEVENT SUMMARY:Black Hole Ringdown Spirals DTSTART:20260212T143000Z DTEND:20260212T160000Z DTSTAMP:20260423T024000Z UID:30167857-515e-428e-9c43-2c3b61856f05 SEQUENCE:1 CREATED:20260211T092429Z DESCRIPTION: The post-merger of a binary black hole coalescence\, known as the ringdown\, provides important information about the remnant black hol e. While dominated by quasi-normal mode emission at early times\, the late time emission is governed by a power-law tail. The amplitude and phase pr operties of the former are found by fitting to numerical relativity wavefo rms\, while the latter are not typically extracted from such simulations d ue to extrapolation artifacts (except in rare cases). Most of these studie s focus on fitting to either the gravitational wave polarizations or ampli tude. In this talk\, I will instead focus on the instantaneous waveform ph ase\, and show how it constitutes an attractor-repulsor system arising fro m the interference between quasi-normal modes and the power-law tail. I wi ll discuss prospects for inferring the properties of the power-law tail in quasi-circular waveforms from numerical relativity\, where they are burie d beneath extraction artifacts. LAST-MODIFIED:20260211T092429Z LOCATION:DF Seminar Room (2-8.3)\, 2nd floor of Physics Building URL:http://df.vps.tecnico.ulisboa.pt/en/events/black-hole-ringdown-spirals / X-ALT-DESC;FMTTYPE=text/html:

The post-merger of a binary black hole coalescence\, known as the ringdown\, provides import ant information about the remnant black hole. While dominated by quasi-nor mal mode emission at early times\, the late time emission is governed by a power-law tail.

The amplitude and phase properties of the forme r are found by fitting to numerical relativity waveforms\, while the latte r are not typically extracted from such simulations due to extrapolation a rtifacts (except in rare cases). Most of these studies focus on fitting to either the gravitational wave polarizations or amplitude.

In th is talk\, I will instead focus on the instantaneous waveform phase\, and s how how it constitutes an attractor-repulsor system arising from the inter ference between quasi-normal modes and the power-law tail. I will discuss prospects for inferring the properties of the power-law tail in quasi-circ ular waveforms from numerical relativity\, where they are buried beneath e xtraction artifacts.

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