Abstract:We consider a class of baryogenesis models where the Lagrangian in the visible sector is ChargeParity (CP ) invariant and a baryon asymmetry is produced only when quantum statistics is taken into account. The CP symmetry is broken by matter effects, namely the assumption that the primordial plasma contains another asymmetric species, such as dark matter. Out-of-equilibrium baryon number violating decays can then generate an asymmetry through Bose enhancement and/or Pauli blocking of certain decay channels.
“…In Ref. [189] we explored an alternative possibility where CP violation is completely sequestered from the other aspects of baryogenesis. We studied the scenario where a particle asymmetry is produced in a dark sector by an unspecified mechanism, leading to a population of an asymmetric, stable species, i.e.…”
The Standard Model of Particle Physics cannot explain the observed baryon asymmetry of the Universe. This observation is a clear sign of new physics beyond the Standard Model. There have been many recent theoretical developments to address this question. Critically, many new physics models that generate the baryon asymmetry have a wide range of repercussions for many areas of theoretical and experimental particle physics. This white paper provides an overview of such recent theoretical developments with an emphasis on experimental testability. Model Key Ingredients Observable scale Observables Axiogenesis Axion misalignment, sphalerons axion scale ~ O( 10 8-11 GeV) axion mass ~ 𝜇eV Gravitational waves WR baryogenesis axion inflation, WR interactions with the inflaton LR symmetry breaking ~ O( 10 10 GeV) Gravitational waves QCD Baryogenesis Singlet scalar coupled to the gluon field strength,
“…In Ref. [189] we explored an alternative possibility where CP violation is completely sequestered from the other aspects of baryogenesis. We studied the scenario where a particle asymmetry is produced in a dark sector by an unspecified mechanism, leading to a population of an asymmetric, stable species, i.e.…”
The Standard Model of Particle Physics cannot explain the observed baryon asymmetry of the Universe. This observation is a clear sign of new physics beyond the Standard Model. There have been many recent theoretical developments to address this question. Critically, many new physics models that generate the baryon asymmetry have a wide range of repercussions for many areas of theoretical and experimental particle physics. This white paper provides an overview of such recent theoretical developments with an emphasis on experimental testability. Model Key Ingredients Observable scale Observables Axiogenesis Axion misalignment, sphalerons axion scale ~ O( 10 8-11 GeV) axion mass ~ 𝜇eV Gravitational waves WR baryogenesis axion inflation, WR interactions with the inflaton LR symmetry breaking ~ O( 10 10 GeV) Gravitational waves QCD Baryogenesis Singlet scalar coupled to the gluon field strength,
“…Compared with the previous works [13,14,22,23], instead of assuming the non-zero PNA at the initial time, the PNA is created through interactions. These interactions have the following unique feature; namely, the interaction between the complex scalars and oscillating condensation of a neutral scalar leads to the PNA.…”
Section: Redshiftmentioning
confidence: 99%
“…For reviews of different types of models and mechanisms, see, for example, [8][9][10]. Recently, the variety of the method for the calculation of BAU has been also developed [11][12][13].…”
A new mechanism for generating particle number asymmetry (PNA) has been developed. This mechanism is realized with a Lagrangian including a complex scalar field and a neutral scalar field.The complex scalar carries U(1) charge which is associated with the PNA. It is written in terms of the condensation and Green's function, which is obtained with two-particle irreducible (2PI) closed time path (CTP) effective action (EA). In the spatially flat universe with a time-dependent scale factor, the time evolution of the PNA is computed. We start with an initial condition where only the condensation of the neutral scalar is non-zero. The initial condition for the fields is specified by a density operator parameterized by the temperature of the universe. With the above initial conditions, the PNA vanishes at the initial time and later it is generated through the interaction between the complex scalar and the condensation of the neutral scalar. We investigate the case that both the interaction and the expansion rate of the universe are small and include their effects up to the first order of the perturbation. The expanding universe causes the effects of the dilution of the PNA, freezing interaction and the redshift of the particle energy. As for the time dependence of the PNA, we found that PNA oscillates at the early time and it begins to dump at the later time. The period and the amplitude of the oscillation depend on the mass spectrum of the model, the temperature and the expansion rate of the universe.
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