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Matter-antimatter Asymmetry in Preheating
Seishi Enomoto | Chengfeng Cai | Zhao-Huan Yu | Hong-Hao Zhang
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Matter-antimatter Asymmetry in Preheating

Seishi Enomoto*, Chengfeng Cai, Zhao-Huan Yu, Hong-Hao Zhang§
School of Physics, Sun Yat-sen University, Guangzhou 510275, China

* seishie@mail.sysu.edu.cn
§ zhh98@mail.sysu.edu.cn


The mechanism of non-perturbative particle production in the preheating era is briefly reviewed. We discuss the possibility of directly generating the matter-antimatter asymmetry through this non- perturbative process. In principle, asymmetry generation is possible if there exists appropriate CP-violating interactions. We show numerical results with a toy model, demonstrating the dynamics. We also show a realistic case in a type-I seesaw model with specific parameters.


In cosmology, inflation and big bang nucleosynthesis (BBN) are strongly supported by current observations. But these two events are not continuous. The temperature of the Universe after inflation would be cold due to the extreme expansion of space, while successful BBN requires a hot Universe with temperatures higher than a few MeV. Moreover, there is no matter-antimatter asymmetry after inflation but only matter appears in the BBN era. Therefore, the Universe must be heated and the asymmetry between matter and the antimatter must be generated by some mechanism after inflation.

A simple story of the (re)heating can be described by the decay of the inflation field into other particles after inflation. Interestingly, however, the "decay" process might be quite different from the normal perturbative picture in some cases [1-4]. To see the specific behavior, let us consider a toy model in which the background field 𝜙 (classical field) is coupled to a real scalar 𝜒 (quantum field), for which the Lagrangian is givern by


where m𝜙 and mχ are masses of 𝜙 and 𝜒 respectively, and g is a coupling constant. For simplicity, we ignore the spatial expansion effect. Especially, in the case of m𝜙 Meff, the decay of 𝜙 into 𝜒 would be forbidden kinematically. This picture is violated if 𝜙 is oscillating with a large amplitude. The actual dynamics solved numerically is shown in Figure 1. As one can see, 𝜒 particles are produced and are growing exponentially despite m𝜙< Meff at all time. An intuitive understanding for why 𝜒 can be produced is that the effective mass of 𝜒, Meff, becomes lighter rapidly around 𝜙 ~ 0, and hence, the kinetic energy of 𝜙 can convert to 𝜒 easily. The exponential evolution of the number density is explained by another reason. Since equations of motion derived from (1) are described by the Mathieu equation, this system can be analogous with a system consisting of a swing (number density of 𝜒) and a person on the swing (amplitude of 𝜙). One can imagine that the person (𝜙) can amplify the amplitude of the swing (𝜒's number density) by crouching down at the moment when the swing passes the lowest point.


Fig. 1: The time evolution of the amplitude of the background field 𝜙 and the number density of 𝜒. We chose the parameters as g = 1 and m𝜙 = mχ = 1013 GeV and 𝜙(t = 0) = 1014 GeV. The particle production occurs around the points of 𝜙~0 (green regions) at which the effective mass of 𝜒 becomes lighter.

This mechanism occurs before the Universe is thermalized, i.e. in the so-called preheating era. Although the analysis is difficult because of the non-perturbative effect, the phenomena are quite interesting. In this article, we introduce its application to the generation of the matter-antimatter asymmetry.


A lot of studies for the generation of the matter-antimatter asymmetry, so-called baryogenesis, have already been carried out. There are several scenarios associated with preheating [5-7]. A motivation for applying non-perturbative particle production is that the parent particles whose decay can generate baryons tend to be heavier than the inflation field. The non-perturbative process allows the creation of heavier particles, while ordinary reheating theory cannot allow it kinematically. Finally, baryons can be obtained by the perturbative decay of such heavy particles.

In the above scenario, is the process to create heavy particles necessary? Naively, even if the heavy particles do not appear, it seems enough that their decay products are produced with asymmetry. In this situation, non-perturbative particle production and asymmetry production seems to occur simultaneously.

The possibility of asymmetry production through non-perturbative particle production has been discussed in earlier studies [8-10]. The essence to generating asymmetry is that the model has a CP-violating interaction. For example, let us consider the following toy model;


where 𝜒 is a complex scalar and is a real scalar, and ϵ and g are complex coupling constants. Note that there is a phase remaining in either ϵ or g after field redefinition. Thus CP is violated in this model. If the mass of 𝜒 oscillates due to another background field 𝜙 as mχ2 = mχ2 (0)+g2 𝜙2 as seen in (1), pairs of particle-antiparticle of 𝜒 would be produced. The actual numerical results shown in Figure 2 support asymmetric production through the non-perturbative process in a case where the model has CP-violating parameters.


As an application of asymmetric production to a realistic situation, it is interesting to consider a Type-I seesaw model that consists of the Standard Model and right-handed neutrinos. In a case where the Higgs background oscillates at a high energy scale, the non-perturbative particle production with a lepton number violating process would occur. Moreover, if the mass scale of the right-handed neutrino is much heavier than the Higgs oscillation scale, the asymmetric production of left-handed neutrinos might occur. Recently our study [11] has shown the possibility of such a scenario. With appropriate parameters, it is possible to explain the baryon asymmetry in the current Universe. The numerical results are shown in Figure 3. One can see that the net lepton number flips when the Higgs background reaches the edge of its oscillation. In the last stage of this dynamics, the Higgs shrinks rapidly at a certain moment because the gauge bosons are also exponentially produced due to the Higgs oscillation. The production of the gauge bosons also stops at a certain moment because their plasma affects the effective mass of the Higgs, and it spoils the motion of the Higgs. Finally, the whole state is fixed, and hence, the lepton-to-entropy ratio is also fixed.

Although the numerical behavior has been shown, it is hard to obtain analytic results because of the difficulty of the analysis of the non-perturbative process. Moreover, our evaluation has not included the expansion effects in the numerical calculation. Although there exist many hurdles to obtaining a complete understanding of the non-perturbative process, we hope these problems could be solved in the future.


Fig. 2: The time evolution of each density. We chose the parameters as m2 = 0.152 + 4cos2 0.03t, m2 = 0.12, and ϵ= 10-4. The upper panel relates to a CP-violating interaction, and the lower panel relates to a CP conserving interaction.


Fig. 3: The time evolution of the lepton-to-entropy ratio, its absolute value with the logarithmic scale and the amplitude of the Higgs background. To perform the calculation, the parameters are set by <h(t0)> = 1.5 횞 1014 GeV and the mass scale of the lightest right-handed neutrino M1 = 1015 GeV. (There are other parameters. See [11] for details.) Δt is a time scale for particle production, which is estimated by Δt ~ [0.1<hmax >]-1 in this parameter set. The final value of the lepton-to-entropy ratio at tt = 100 is nL/s = -6.54횞10-10.

Acknowledgments: This work is supported in part by the National Natural Science Foundation of China under Grant Nos. 11805288, 11875327, and 11905300, the China Postdoctoral Science Foundation under Grant No. 2018M643282, the Natural Science Foundation of Guangdong Province under Grant No. 2016A030313313, the Fundamental Research Funds for the Central Universities, and the Sun Yat-Sen University Science Foundation. A part of this study was performed in collaboration with Prof. T. Matsuda at Saitama Institute of Technology.


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Seishi Enomoto is a research fellow at the Particle Physics Theory Group, School of Physics, Sun Yat-sen University in Guangzhou, China. He received his PhD degree in 2013 from Nagoya University for his study of theoretical particle physics and cosmology. His current research interests include inflation theory, reheating theory after inflation, non-perturbative effect in quantum field theory.

Chengfeng Cai is a postdoc at the Particle Physics Theory Group, the School of Physics, Sun Yat-sen University in Guangzhou, China. He received his PhD degree in 2017 from the School of Physics, Sun Yat-sen University. He continued his study as a postdoc at Sun Yat-sen University. His current research interests include new physics beyond standard model phenomenology and cosmology.

Zhao-Huan Yu is an associate professor of physics at the School of Physics, Sun Yat-sen University, Guangzhou, China. He received his PhD degree in 2015 from Institute of High Energy Physics, Chinese Academy of Sciences. He continued his research as a postdoc at the School of Physics, the University of Melbourne until he joined Sun Yat-sen University in 2018. His study focuses on dark matter phenomenology and collider physics.

Hong-Hao Zhang is a professor of physics at the School of Physics, Sun Yat-sen University in Guangzhou, China. He received his PhD degree in 2007 from Physics Department, Tsinghua University in Beijing. Thereafter he worked as a faculty member at the Sun Yat-sen University in Guangzhou. He was promoted to a full professor in January 2017. His research focuses on quantum field theory, particle physics and cosmology.

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