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SUMMARY:Learning more from Kerr - New tools and related results
DTSTART:20230223T143000Z
DTEND:20230223T160000Z
DTSTAMP:20260801T171552Z
UID:547986be-7efb-423d-b08d-3573ee86de27
SEQUENCE:1
CREATED:20230220T102015Z
DESCRIPTION:ABSTRACT: There is good reason to think that gravitational wav
 e physics\, and particularly single black hole perturbation theory\, is at
  a turning point. In this talk\, I will review some of the challenges curr
 ently facing our understanding of single perturbed black holes. The settin
 g of this review will be gravitational waves from the merger of stellar ma
 ss binary black holes (BBHs)\, and related conceptual tensions. I will pay
  particular attention to the relevance of Kerr “quasi-normal modes” (Q
 NMs) to BBH merger\, and I will discuss how our burgeoning understanding o
 f QNM orthogonality points the way to new directions of research. As an ex
 ample\, I will present a proof-of-concept for a purely spectral method of 
 solving Teukoslky’s radial equation. 
LAST-MODIFIED:20230220T102015Z
LOCATION:Sala de Seminários do DF\,  Pavilhão de Física\, 2º piso
URL:http://df.vps.tecnico.ulisboa.pt/pt/eventos/learning-more-from-kerr-ne
 w-tools-and-related-results/
X-ALT-DESC;FMTTYPE=text/html:<p data-block-key="8qnl8"><b>ABSTRACT: </b></
 p><p data-block-key="1r5jo">There is good reason to think that gravitation
 al wave physics\, and particularly single black hole perturbation theory\,
  is at a turning point. In this talk\, I will review some of the challenge
 s currently facing our understanding of single perturbed black holes. <br/
 ><br/>The setting of this review will be gravitational waves from the merg
 er of stellar mass binary black holes (BBHs)\, and related conceptual tens
 ions. I will pay particular attention to the relevance of Kerr “quasi-no
 rmal modes” (QNMs) to BBH merger\, and I will discuss how our burgeoning
  understanding of QNM orthogonality points the way to new directions of re
 search. As an example\, I will present a proof-of-concept for a purely spe
 ctral method of solving Teukoslky’s radial equation. </p>
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