Gravitational waves from dark SU(3) Yang-Mills theory

Morgante, Enrico; Ramberg, Nicklas; Schwaller, Pedro

doi:10.1103/physrevd.107.036010

Cited by 33 publications

(10 citation statements)

References 88 publications

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“…In agreement with the results therein, we find β /H = O 10 4 − 10 5 for all models. Similar results are obtained for both chiral and confinement/deconfinement phase transitions in holographic studies [22,25] of strongly coupled theories. These values are orders of magnitude larger compared to the inverse timescale of cosmological phase transitions in non-strongly interacting models, where typically β /H = O (100).…”

Section: Gravitational Wave Backgroundsupporting

confidence: 83%

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Supercool exit: Gravitational waves from QCD-triggered conformal symmetry breaking

Sagunski¹,

Schicho²,

Schmitt³

2023

Preprint

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Section: Gravitational Wave Backgroundsupporting

confidence: 83%

“…originate from a cosmological first-order phase transition (PT) [5][6][7][8], as predicted by many theories beyond the Standard Model (SM). Examples of such theories are scalar SM extensions [9][10][11][12][13][14][15][16][17][18] or secluded dark sectors [19][20][21][22][23][24][25].…”

Section: Introductionmentioning

confidence: 99%

Supercool exit: Gravitational waves from QCD-triggered conformal symmetry breaking

Sagunski¹,

Schicho²,

Schmitt³

2023

Preprint

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“…Typically, the duration of the phase transition is expected to be some fraction of Hubble, H, with β/H between 100 − 10 5 . Here 100 is the maximal possible value [75], while 10 5 is a value suggested by a holographic computation [69]. Note the larger value of β/H (i.e., a shorter duration phase transition) gives rise to a smaller amplitude in Ω GW h 2 but also a higher peak frequency of f c or f t .…”

Section: Gravitational Waves From Su (3) Phase Transitionmentioning

confidence: 99%

“…The precise value of α is not as important since the spectrum is fairly insensitive to α as long as it is O(1). For a fiducial value, we take α 0.343 [69]. Last, we assume that the efficiency factor is the same for collisions, turbulence, and sound waves.…”

Section: Gravitational Waves From Su (3) Phase Transitionmentioning

confidence: 99%

A Heavy QCD Axion and the Mirror World

Dunsky¹,

Hall²,

Harigaya³

2023

Preprint

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We study the mirror world with dark matter arising from the thermal freezeout of the lightest, stable mirror particle -the mirror electron. The dark matter abundance is achieved for mirror electrons of mass 225 GeV, fixing the mirror electroweak scale near 10 8 GeV. This highly predictive scenario is realized by an axion that acts as a portal between the two sectors through its coupling to the QCD and mirror QCD sectors. The axion is more massive than the standard QCD axion due to additional contributions from mirror strong dynamics. Still, the strong CP problem is solved by this 'heavy' axion due to the alignment of the QCD and mirror QCD potentials. Mirror entropy is transferred into the Standard Model sector via the axion portal, which alleviates overproduction of dark radiation from mirror glueball decays. This mirror scenario has a variety of signals: (1) primordial gravitational waves from the first-order mirror QCD phase transition occurring at a temperature near 35 GeV, (2) effects on large-scale structure from dark matter self-interactions from mirror QED, (3) dark radiation affecting the cosmic microwave background, and (4) the rare kaon decay, K + → (π + + axion). The first two signals do not depend on any fundamental free parameters of the theory while the latter two depend on a single free parameter, the axion decay constant.

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“…The LTE approximation is shown to work well for strongly coupled theories [81] whose FOPT-related phenomenology has been studied in, e.g., refs. [66,[88][89][90][91][92][93][94][95][96][97][98][99][100].…”

Section: Jcap03(2024)037mentioning

confidence: 99%

Criterion for ultra-fast bubble walls: the impact of hydrodynamic obstruction

Ai,

Nagels,

Vanvlasselaer

2024

J. Cosmol. Astropart. Phys.

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The Bödeker-Moore thermal friction [1] is usually used to determine whether or not a bubble wall can run away. However, the friction on the wall is not necessarily a monotonous function of the wall velocity and could have a maximum before it reaches the Bödeker-Moore limit. In this paper, we compare the maximal hydrodynamic obstruction, a frictional force that exists in local thermal equilibrium, and the Bödeker-Moore thermal friction. We study the former in a fully analytical way, clarifying its physical origin and providing a simple expression for its corresponding critical phase transition strength above which the driving force cannot be balanced out by the maximal hydrodynamic obstruction. We find that for large parameter space, the maximal hydrodynamic obstruction is larger than the Bödeker-Moore thermal friction, indicating that the conventional criterion for the runaway behavior of the bubble wall may have to be modified. We also explain how to apply efficiently the modified criterion to particle physics models and discuss possible limitations of the analysis carried out in this paper.

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Gravitational waves from dark SU(3) Yang-Mills theory

Cited by 33 publications

References 88 publications

Supercool exit: Gravitational waves from QCD-triggered conformal symmetry breaking

Supercool exit: Gravitational waves from QCD-triggered conformal symmetry breaking

A Heavy QCD Axion and the Mirror World

Criterion for ultra-fast bubble walls: the impact of hydrodynamic obstruction

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