Gravitational waves from first-order phase transitions: from weak to strong

被引:0
作者
Caprini, Chiara [1 ,2 ]
Jinno, Ryusuke [3 ]
Konstandin, Thomas [4 ]
Pol, Alberto Roper [1 ]
Rubira, Henrique [5 ]
Stomberg, Isak [4 ,6 ]
机构
[1] Univ Geneva, Dept Phys Theor, CH-1211 Geneva, Switzerland
[2] CERN, Theoret Phys Dept, CH-1211 Geneva, Switzerland
[3] Kobe Univ, Dept Phys, Kobe 6578501, Japan
[4] Deutsch Elektronen Synchrotron DESY, Notkestr 85, D-22607 Hamburg, Germany
[5] Tech Univ Munich, Phys Dept T31, James Franck Str 1, D-85748 Garching, Germany
[6] Univ Valencia, IFIC, CSIC, C Catedrat Jose Beltran 2, E-46980 Paterna, Spain
基金
瑞士国家科学基金会;
关键词
Phase Transitions in the Early Universe; Cosmology of Theories BSM; BARYON-NUMBER NONCONSERVATION; FALSE VACUUM; RADIATION; PROGRESS; BUBBLES; GROWTH; FATE;
D O I
10.1007/JHEP07(2025)217
中图分类号
O412 [相对论、场论]; O572.2 [粒子物理学];
学科分类号
摘要
We study the generation of gravitational waves (GWs) during a cosmological first-order phase transition (PT) using the recently introduced Higgsless approach to numerically simulate the fluid motion induced by the PT. We present for the first time GW spectra sourced by bulk fluid motion in the aftermath of strong first-order PTs (alpha = 0.5), alongside weak (alpha = 0.0046) and intermediate (alpha = 0.05) PTs, previously considered in the literature. We find that, for intermediate and strong PTs, the kinetic energy in our simulations decays, following a power law in time. The decay is potentially determined by non-linear dynamics and hence related to the production of vorticity. We show that the assumption that the source is stationary in time, characteristic of compressional motion in the linear regime (sound waves), agrees with our numerical results for weak PTs, since in this case the kinetic energy does not decay with time. We then provide a theoretical framework that extends the stationary assumption to one that accounts for the time evolution of the source: as a result, the GW energy density is no longer linearly increasing with the source duration, but proportional to the integral over time of the squared kinetic energy fraction. This effectively reduces the linear growth rate of the GW energy density and allows to account for the period of transition from the linear to the non-linear regimes of the fluid perturbations. We validate the novel theoretical model with the results of simulations and provide templates for the GW spectrum for a broad range of PT parameters.
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页数:69
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