Gravitational Radiation from First-Order Phase Transitions

Details Gravitational Radiation from First-Order Phase Transitions Gravitational Radiation from First-Order Phase Transitions

1993-10-25

arxiv.org/abs/astro-ph/9310044v1

Phys.Rev. D49 (1994) 2837-2851

Astronomy and Astrophysics

Astrophysics

(25 pages and 9 figures as one uuencoded PostScript file), IASSNS-HEP-93/44, FNAL-Pub-235-A

Scientific paper

10.1103/PhysRevD.49.2837

We consider the stochastic background of gravity waves produced by first-order cosmological phase transitions from two types of sources: colliding bubbles and hydrodynamic turbulence. First we discuss the fluid mechanics of relativistic spherical combustion. We then numerically collide many bubbles expanding at a velocity $v$ and calculate the resulting spectrum of gravitational radiation in the linearized gravity approximation. Our results are expressed as simple functions of the mean bubble separation, the bubble expansion velocity, the latent heat, and the efficiency of converting latent heat to kinetic energy of the bubble walls. We also estimate the gravity waves produced by a Kolmogoroff spectrum of turbulence and find that the characteristic amplitude of gravity waves produced is comparable to that from bubble collisions. Finally, we apply these results to the electroweak transition. Using the one-loop effective potential for the minimal electroweak model, the characteristic amplitude of gravity waves produced is $h\simeq 1.5\times 10^{-27}$ at a characteristic frequency of $4.1\times 10^{-3} \,\rm Hz$ corresponding to $\Omega \sim10^{-22}$ in gravity waves, far too small for detection. Gravity waves from more strongly first-order phase transitions, including the electroweak transition in non-minimal models, have better prospects for detection, though probably not by LIGO.

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