Induced gravitational waves as a cosmological probe of the sound speed during the QCD phase transition

• Published in: arXiv.org
• Main Authors: Abe, Katsuya T, Tada, Yuichiro, Ueda, Ikumi
• Format: Paper Journal Article
• Language: English
• Published: Ithaca Cornell University Library, arXiv.org 13.10.2020
• Subjects: Arrays; Astronomical models; Cosmology; Equations of state; Frequency ranges; Gravitation; Gravitational waves; Invariants; Particle physics; Perturbation; Phase transitions; Physics - Cosmology and Nongalactic Astrophysics; Physics - High Energy Physics - Phenomenology; Plasmas (physics); Pulsars; Quantum chromodynamics; Sound; Standard model (particle physics); Wave propagation
• ISSN: 2331-8422
• DOI: 10.48550/arxiv.2010.06193

The standard model of particle physics is known to be intriguingly successful. However their rich phenomena represented by the phase transitions (PTs) have not been completely understood yet, including the possibility of the existence of unknown dark sectors. In this Letter, we investigate the measurement of the equation of state parameter \(w\) and the sound speed \(c_{\rm s}\) of the PT plasma with use of the gravitational waves (GWs) of the universe. Though the propagation of GW is insensitive to \(c_{\rm s}\) in itself, the sound speed value affects the dynamics of primordial density (or scalar curvature) perturbations and the induced GW by their horizon reentry can then be an indirect probe both \(w\) and \(c_{\rm s}\). We numerically reveal the concrete spectrum of the predicted induced GW with two simple examples of the scalar perturbation spectrum: the monochromatic and scale-invariant spectra. In the monochromatic case, we see that the resonant amplification and cancellation scales of the induced GW depend on the \(c_{\rm s}\) values at different time respectively. The scale-invariant case gives a more realistic spectrum and its specific shape will be compared with observations. In particular, the QCD phase transition corresponds with the frequency range of the pulsar timing array (PTA) observations. If the amplitude of primordial scalar power is in the range of \(10^{-4}\lesssim A_\zeta\lesssim10^{-2}\), the induced GW is consistent with current observational constraints and detectable in the future observation in Square Kilometer Array. Futhermore the recent possible detection of stochastic GWs by NANOGrav 12.5 yr analysis~[1] can be explained by the induced GW if \(A_\zeta\sim\sqrt{7}\times10^{-3}\).