2002/02/20 by J C N de Araujo, O D Miranda, O D Aguiar
Physics and Astronomy · #Amplitude #Black hole (networking) #Cosmology and Gravitation Theories #Gravitational wave #Gravitational wave background #Particle physics theoretical and experimental studies #Population #Primordial black hole #Pulsars and Gravitational Waves Research #Redshift #Stellar black hole #astro-ph #gr-qc
paper · pdf · doi:10.1088/0264-9381/19/7/315
published as Class.Quant.Grav. 19 (2002) 1335-1342 · 9 pages (IOPP Latex2e), 1 eps figure; To appear in Classical an Quantum Gravity (Special Issue: Proceedings of the 4th Edoardo Amaldi Conference on Gravitational Waves)
arxiv created 2002/02/20 · openalex publication_date 2002/03/12 · arxiv updated 2009/11/30 · openalex created_date 2016/06/24 · openalex updated_date 2026/08/05
We study the generation of a gravitational wave (GW) background produced from a population of core-collapse supernovae, which form black holes in scenarios of structure formation of the Universe. We obtain, for example, that a pre-galactic population of black holes, formed at redshifts z≃ 30-10, could generate a stochastic GW background with a maximum amplitude of h\rm BG≃ 10-24 in the frequency band ν\rm obs≃ 30-470 \rm Hz (considering a maximum efficiency of generation of GWs, namely, ε\rm GW=7× 10-4). In particular, we discuss what astrophysical information could be obtained from a positive, or even a negative, detection of such a GW background produced in scenarios such as those studied here. One of them is the possibility of obtaining the initial and final redshifts of the emission period from the observed spectrum of GWs.