Gravitational Wave Background from Population III Stars
Abstract
We estimate the gravitational wave (GW) background from Population III (Pop III) stars using the results from our hydrodynamic simulations (Suwa et al. 2007). We calculate gravitational waveforms from matter motions and anisotropic neutrino emissions for single Pop III stars. We find that the GW amplitudes from matter motions are dominant until just after bounce, but those from neutrinos dominate later on at frequencies below Hz in the GW spectrum. Computing the overall signal produced by the ensemble of such Pop III stars, we find that the resultant density parameter of the GW background peaks at the amplitude of in the frequency interval Hz. We show that such signals, depending on the formation rate of Pop III stars, can be within the detection limits of future planned interferometers such as DECIGO and BBO in the frequency interval of Hz. Our results suggest that the detection of the GW background from Pop III stars can be an important tool to supply the information about the star formation history in the early universe.
Cite
@article{arxiv.0706.3495,
title = {Gravitational Wave Background from Population III Stars},
author = {Yudai Suwa and Tomoya Takiwaki and Kei Kotake and Katsuhiko Sato},
journal= {arXiv preprint arXiv:0706.3495},
year = {2010}
}