CosmoTransitions: Computing cosmological phase transition temperatures and bubble profiles with multiple fields

Wainwright, Carroll L.

doi:10.1016/j.cpc.2012.04.004

Cited by 435 publications

(399 citation statements)

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“…Equivalently, the bounce solution of the Euclidean action is a minimum of the action with respect to deformations of fixed, one-dimensional paths in the field space. The implication of this result is that the path deformation method of CosmoTransitions (CT) [45] is guaranteed to provide at least an upper bound on the tunnelling lifetime.…”

Section: A Minimality Of the Action Under Path Deformationsmentioning

confidence: 99%

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Vacuum stability and the MSSM Higgs mass

Blinov

Morrissey

2014

J. High Energ. Phys.

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In the Minimal Supersymmetric Standard Model (MSSM), a Higgs boson mass of 125 GeV can be obtained with moderately heavy scalar top superpartners provided they are highly mixed. The source of this mixing, a soft trilinear stop-stop-Higgs coupling, can result in the appearance of charge-and color-breaking minima in the scalar potential of the theory. If such a vacuum exists and is energetically favorable, the Standard Model-like vacuum can decay to it via quantum tunnelling. In this work we investigate the conditions under which such exotic vacua arise, and we compute the tunnelling rates to them. Our results provide new constraints on the scalar top quarks of the MSSM.

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Section: A Minimality Of the Action Under Path Deformationsmentioning

confidence: 99%

“…Several methods of solving the multi-field bounce equation of motion have been proposed [25,[42][43][44]. In the present analysis we use the public code CosmoTransitions [45]. 1 CosmoTransitions (CT) implements a path deformation method similar to the that suggested in ref.…”

Section: Jhep03(2014)106mentioning

confidence: 99%

Vacuum stability and the MSSM Higgs mass

Blinov

Morrissey

2014

J. High Energ. Phys.

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“…In other words, the Universe is in a supercooled state for some time. To calculate the nucleation temperatures T S and T n we used the publicly available CosmoTransitions package [23][24][25][26]. Note that since the effective potential is gauge dependent away from the minima, the calculated T n may have a residual gauge dependence, see e.g.…”

mentioning

confidence: 99%

Dark Matter Decay between Phase Transitions at the Weak Scale

Baker

Kopp

2017

Phys. Rev. Lett.

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We propose a new alternative to the Weakly Interacting Massive Particle (WIMP) paradigm for dark matter. Rather than being determined by thermal freeze-out, the dark matter abundance in this scenario is set by dark matter decay, which is allowed for a limited amount of time just before the electroweak phase transition. More specifically, we consider fermionic singlet dark matter particles coupled weakly to a scalar mediator S3 and to auxiliary dark sector fields, charged under the Standard Model gauge groups. Dark matter freezes out while still relativistic, so its abundance is initially very large. As the Universe cools down, the scalar mediator develops a vacuum expectation value (vev), which breaks the symmetry that stabilises dark matter. This allows dark matter to mix with charged fermions and decay. During this epoch, the dark matter abundance is reduced to give the value observed today. Later, the SM Higgs field also develops a vev, which feeds back into the S3 potential and restores the dark sector symmetry. In a concrete model we show that this "vev flip-flop" scenario is phenomenologically successful in the most interesting regions of its parameter space. We also comment on detection prospects at the LHC and elsewhere.The WIMP (Weakly Interacting Massive Particle) paradigm in dark matter physics states that dark matter (DM) particles should have non-negligible couplings to Standard Model (SM) particles. Their abundance today would then be determined by their abundance at freeze-out, the time when the temperature of the Universe dropped to the level where interactions producing and annihilating DM particles become inefficient. In many models these interactions should still be observable today, through residual DM annihilation in galaxies and galaxy clusters, through scattering of DM particles on atomic nuclei, or through DM production at colliders. The conspicuous absence of any convincing signals [1][2][3][4][5][6][7] to date motivates us to look for alternatives to the WIMP paradigm.In this letter, we present a scenario in which the DM abundance is set not by annihilation, but by decay. We focus on models in which fermionic DM particles couple to a new scalar species and argue that the resulting scalar potential may undergo multiple phase transitions, "flip-flopping" between phases in which the symmetry stabilising the DM is intact and a phase where it is broken. Similar behaviour is found in models of electroweak baryogenesis [8][9][10][11][12][13][14], see also [15] for related work. During the broken phase, the initially overabundant DM particles are depleted until their relic density reaches the value observed today. Although the resulting picture of early freeze out, followed by a period of DM decay around the weak scale, is quite generic, we focus here on a concrete example and comment on possible generalisations in the end.Model Framework.-We introduce a complex dark sector scalar S 3 that is a triplet under the SM SU (2) L gauge symmetry and carries zero hypercharge. We take the DM particle to...

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“…In absence of global CCB minima the SML vacuum is stable. If the global minima is found to break the charge and color symmetry, the code computes the lifetime of the SML minima against decay to the global CCB minima using the code CosmoTransitions [37]. It then determines whether the SML minima is long-lived or short-lived.…”

Section: Jhep11(2014)161mentioning

confidence: 99%

“…This may even put more stringent constraints than what are actually required [30][31][32][33]35]. Hence, for a given point in the multi-dimensional parameter space it is important to check the existence of any deeper CCB minima numerically as exhaustively performed in codes like Vevacious (version 1.0.11) [36] that in turn uses CosmoTransitions [37]. In case such minima exist one should compute the lifetime of the false vacuum and decide on the validity of the given point of parameter space depending on the computed lifetime.…”

Section: Jhep11(2014)161mentioning

confidence: 99%

Exploring MSSM for charge and color breaking and other constraints in the context of Higgs@125 GeV

Chattopadhyay

Dey

2014

J. High Energ. Phys.

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Exploring MSSM parameter space after the discovery of Higgs Boson at 125 GeV naturally demands large top-squark mixing or large trilinear coupling parameter A t in particular, so as to avoid excessively heavy squark, specially for the universal models like CMSSM. We study stability of electroweak symmetry breaking vacua in possible presence of deeper charge-color symmetry breaking minima within MSSM. Besides stable vacua, we consider scenarios characterized by the presence of global CCB minima, with SM like charge and color conserving vacuum, having stability over cosmologically large lifetime (long-lived states). We allow vacuum expectation values for both stop as well as sbottom fields, since these belong to the third generation of sfermions with larger Yukawa couplings that have immediate effect on the tunneling time. Moreover, for large µ regions, radiative corrections to Higgs boson mass from bottom-squark loop is quite significant. Regions of MSSM parameters space become viable for large A t and large µ zones which are generically excluded via the traditional analytical CCB constraints. For a large value of tan β, safe vacua associated with large values of |µ| and |A t | are predominantly long-lived and may be associated with relatively light stop masses. We also identify low µ regions associated with long-lived states. Both the above zones can be friendly to muon g − 2 constraint. We also impose constraints from Br(B → X s γ) and Br(B s → µ + µ − ). We do the analysis for a moderate and a large tan β. We choose an example parameter point in the gaugino mass plane of M 1 , M 2 that satisfies the dark matter constraints, basically a decoupled sector with respect to CCB.

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CosmoTransitions: Computing cosmological phase transition temperatures and bubble profiles with multiple fields

Cited by 435 publications

References 46 publications

Vacuum stability and the MSSM Higgs mass

Vacuum stability and the MSSM Higgs mass

Dark Matter Decay between Phase Transitions at the Weak Scale

Exploring MSSM for charge and color breaking and other constraints in the context of Higgs@125 GeV

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