Advances and Challenges in Computational Relativity Sep 14-18, 2020 Testing the nature of dark compact objects with gravitational waves Elisa Maggio Sapienza University of Rome https://web.uniroma1.it/gmunu
Gravitational waves from binary mergers Up to date 15 gravitational wave events from the coalescence of compact binaries have been detected. The signal has 3 stages: • Inspiral • Merger • Ringdown Abbott+, PRL 116 , 061102 (2016) Elisa Maggio Testing dark compact objects with GWs @ICERM 2020 1/21
Gravitational waves from binary mergers Up to date 15 gravitational wave events from the coalescence of compact binaries have been detected. The signal has 3 stages: • Inspiral • Merger • Ringdown What is the nature of the Abbott+, PRL 116 , 061102 (2016) compact remnant? Elisa Maggio Testing dark compact objects with GWs @ICERM 2020 1/21
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sha1_base64="xFAtIKVixsdGp32F8kEca74j4N0=">ACIHicbVDLSgNBEJz1bXxFPXoZDIHDbsimIsgeNGbglEhG5beScOzswuM71iWPYn/AS/wquevIlHBf/FTczBV52Kqm6q+JUSUe+/+aNjU9MTk3PzFbm5hcWl6rLK+cuyazApkhUYi9jcKikwSZJUniZWgQdK7yIrw8H/sUNWicTc0b9FNsaekZ2pQAqpai6FRJkUR4S3lLeAZ1K0ysKvs+3edi1IPKgyMNEYw+i4yKq1vy6PwT/S4IRqbERTqLqR9hJRKbRkFDgXCvwU2rnYEkKhUlzBymIK6h62SGtDo2vkwVcE3MgeU8BQtl4oPRfy+kYN2rq/jclIDXbnf3kD8z2tl1G20c2nSjNCIwSGSCoeHnLCyrAt5R1okgsHnyKXhAiwQoZUchCjFrOyvUvYR/E7/l5zv1AO/Hpzu1g4ao2Zm2BpbZ5sYHvsgB2xE9Zkgt2xB/bInrx79l78V6/Rse80c4q+wHv/RNLY6PE</latexit> Ringdown stage The ringdown stage is dominated by the quasi-normal modes of the remnant which describe the response of the compact object to a perturbation. ω = ω R + i ω I The signal can be modeled as a sum of exponentially damped sinusoids: f GW | ringdown = ω R 2 π τ damping = − 1 ω I Buonanno, CQG 19 , 1267-1278 (2002) Elisa Maggio Testing dark compact objects with GWs @ICERM 2020 2/21
Ringdown detections The least-damped quasi-normal mode has been observed in the ringdown of the events GW150914 and GW190521. Both detections are compatible with Kerr black hole remnants . GW150914 GW190521 Abbott+, PRL 116 , 221101 (2016) Abbott+, ApJL 900 , L13 (2020) However, the characterization of the remnant is still an open problem . Elisa Maggio Testing dark compact objects with GWs @ICERM 2020 3/21
Test of the BH paradigm A test of the no-hair theorem requires the identification of at least two QNM frequencies in the ringdown. Dreyer+, CQG 21 , 787 (2004) Kerr black holes are uniquely determined by 2 parameters: • Mass • Angular momentum Carter, PRL 26 , 331 (1971); Robinson, PRL 34 , 905 (1975) Louder GW events and improvements of the detector sensitivity will allow to test the BH hypothesis. Berti, Cardoso, Will, PRD 73 , 064030 (2006) Elisa Maggio Testing dark compact objects with GWs @ICERM 2020 4/21
Questions I. Are there alternative models to black holes? II. Are they astrophysically viable? III. What is the gravitational wave signal that they produce? IV. Is their gravitational wave signal detectable? Elisa Maggio Testing dark compact objects with GWs @ICERM 2020 5/21
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