Baryon asymmetry in the inflationary universe

It is shown that the baryon asymmetry in the inflationary universe under certain constraints on the masses of superheavy bosons can be larger than that in the standard baryosynthesis scenario. An important property of the model considered is that the final baryon asymmetry does not depend on initial conditions in the early universe in contrast to what occurs in the standard scenario based on B?L conserving GUTs.     

Baryogenesis via density fluctuations with a second-order electroweak phase transition

We consider the presence of cosmic string-induced density fluctuations in the early universe at temperatures below the electroweak phase transition temperature. Resulting temperature fluctuations can restore the electroweak symmetry locally, depending on the amplitude of fluctuations and the background temperature. The symmetry will be spontaneously broken again in a given region as the temperature drops there (for fluctuations with length scales smaller than the horizon), resulting in the production of baryon asymmetry. The time-scale of the transition will be governed by the wavelength of fluctuation and, hence, can be much smaller than the Hubble time. This leads to strong enhancement in the production of baryon asymmetry for a second-order electroweak phase transition as compared to the case when transition happens due to the cooling of the universe via expansion. For a two-Higgs doublet model (with appropriate CP violation), we show that one can get the required baryon asymmetry if fluctuations propagate without getting significantly damped. If fluctuations are damped rapidly, then a volume factor suppresses the baryon production, though it is still 3–4 orders of magnitude larger than the conventional case of second-order transition.     

The development of baryon asymmetry in the early universe

The development of an excess of baryons over antibaryons due to CP and baryon number violating reactions during the very early stages of the big bang is calculated in simple models using the Boltzmann equation. We show that it is necessary to solve the coupled Boltzmann equations in order to determine the final baryon number in any specific model.     

Baryon asymmetry generation through preonic monopoles

A scheme is presented for baryon asymmetry generation in early universe through monpole-induced baryon number violating processes in the context of a preonic model.     

Baryon asymmetry and low energy parity restoration

We examine the question of baryon number generation in the early universe in theories with low intermediate mass scales It is shown that the recently proposed O(10) grand unified theory with parity restoration at E ≈ few hundred GeV allows for the creation of matter-antimatter asymmetry in accord with cosmological observations. This evades a recent general argument for incompatibility between weakly broken left-right symmetry and substantial baryon generation.     

Baryogenesis in false vacuum

The null result in the LHC may indicate that the standard model is not drastically modified up to very high scales, such as the GUT/string scale. Having this in the mind, we suggest a novel leptogenesis scenario realized in the false vacuum of the Higgs field. If the Higgs field develops a large vacuum expectation value in the early universe, a lepton number violating process is enhanced, which we use for baryogenesis. To demonstrate the scenario, several models are discussed. For example, we show that the observed baryon asymmetry is successfully generated in the standard model with higher-dimensional operators.     

High-energy gravity and the very early universe

It is suggested that gravity may not be asymptotically free at short distances because of the interaction of the graviton with matter. If gravity indeed becomes strong at high energies, a revolutionary change of our present theory on the early universe would seem to be necessary. During the first extremely small fraction of a second in the big-bang universe, gravity would have been so strong that it might not have been described by Einstein's theory of general relativity. The possibility of abnormally strong gravity at high energies or short distances is discussed in some detail. A possible explanation is proposed for the nonvanishing mean baryon number density of the universe. It is also pointed out that the universe may well escape from the catastrophic singularity of Penrose and Hawking.     

Cosmological implications of observable neutron-antineutron oscillations

A wide class of gauge theoretical models allowing for observable neutron-antineutron oscillations predict no baryon asymmetry in the present universe. This is to be traced back to the existence of baryon-violating interactions in equilibrium at the characteristic mass scale of neutron-antineutron oscillations. Then, we show how these models can be modified in such a way that a very late cosmological baryon asymmetry survives in the today universe. Specifically, we consider two recently proposed baryon-production mechanisms, one of which can be naturally embedded in a grand unification scheme and can lead to observable nucleon decay processes occurring only throughB-L violating butB+L conserving channels.     

Baryon asymmetry, inflation and squeezed states

We use the general formalism of squeezed rotated states to calculate baryon asymmetry in the wake of inflation through parametric amplification. We base our analysis on a B and CP violating Lagrangian in an isotropically expanding universe. The B and CP violating terms originate from the coupling of complex fields with non-zero baryon number to a complex background inflaton field. We show that a differential amplification of particle and antiparticle modes gives rise to baryon asymmetry.     

宇宙中的光子数、重子数、及反重子数

在粒子物理与宇宙学二者的结合上,近年已经取得了颇有意义的进展。重子不对称和重子光子数比的起源可以用大统一理论加以解释。由B、C及CP破坏的相互作用可以说明为什么初始重子对称的宇宙能演化成不对称的。目前观测到的重子光子数比10~(-9)可能是由极早期宇宙中的超重玻色子的衰变产生的,在这种衰变中C及CP是破坏的。尽管衰变解释是吸引入的,但它的具体预言很强地依赖于超重玻色子的质量,以致其数值尚不确定。因此。为了进一步考查衰变模型的合理性,至少还要研究其他的可能有影响的过程。在这个意义下,本文还讨论了宇宙早期中的Higgs相变对重子光子比的影响。     

Time's arrow in an oscillating universe

In view of the time-symmetric nature of the laws of physics, time asymmetry in the universe must arise from “initial” conditions. A fully time-symmetric oscillating model is presented which exists in a highly compressed, highly ordered state att=0 and evolves forward, in the thermodynamic sense, as ∣t ∣ increases. This model offers the possibility of accounting for several fundamental and puzzling aspects of our universe, including matter-antimatter asymmetry, the large entropy per baryon, primordial density enhancements sufficient to form galaxies, and large-scale homogeneity.     

Confronting dark energy models mimicking ΛCDM epoch with observational constraints: Future cosmological perturbations decay or future Rip?

We confront dark energy models which are currently similar to ΛCDM theory with observational data which include the SNe data, matter density perturbations and baryon acoustic oscillations data. DE cosmology under consideration may evolve to Big Rip, type II or type III future singularity, or to Little Rip or Pseudo-Rip universe. It is shown that matter perturbations data define more precisely the possible deviation from ΛCDM model than consideration of SNe data only. The combined data analysis proves that DE models under consideration are as consistent as ΛCDM model. We demonstrate that growth of matter density perturbations may occur at sufficiently small background density but still before the possible disintegration of bound objects (like clusters of galaxies, galaxies, etc.) in Big Rip, type III singularity, Little Rip or Pseudo-Rip universe. This new effect may bring the future universe to chaotic state well before disintegration or Rip.     

The baryon asymmetry and CPT invariance in the early universe

We discuss, and give a definite, simple phenomenological example, of the possibility that the baryon asymmetry is related to a failure of CPT invariance for a brief time interval at the origin of the universe.     

Models of neutrino masses and baryogenesis

Majorana masses of the neutrino implies lepton number violation and is intimately related to the lepton asymmetry of the universe, which gets related to the baryon asymmetry of the universe in the presence of the sphalerons during the electroweak phase transition. Assuming that the baryon asymmetry of the universe is generated before the electroweak phase transition, it is possible to discriminate different classes of models of neutrino masses. While see-saw mechanism and the triplet Higgs mechanism are preferred, the Zee-type radiative models and the R-parity breaking models requires additional inputs to generate baryon asymmetry of the universe during the electroweak phase transition.     

Dark matter and the baryon asymmetry of the universe

We present a mechanism to generate the baryon asymmetry of the Universe which preserves the net baryon number created in the big bang. If dark matter particles carry baryon number Bx, and sigmaxannih相似文献   

Electroweak baryon number violation at finite temperature

We consider baryon and lepton number violating processes in the electroweak theory induced by gauge and Higgs fields passing the sphaleron solution at finite temperature. We show that for temperatures larger than 19 GeV the anomalous baryon and lepton number violating processes are suppressed by the Boltzmann factor exp (?βE _sp), whereE _sp is the sphaleron energy, rather than by the instanton tunneling factor exp (?8π²/g ²). We caculate the rate of baryon and lepton number violating processes at finite temperature and determine the freezing temperature of the anomalous processes in the early universe as a function of the Higgs mass. We compare the freezing temperature with the critical temperature of the electroweak phase transition infered from the one-loop finite-temperature effective potential. We obtain a critical Higgs mass of the order of 100 GeV, slightly depending on the top mass and the magnitude of the pre-exponential factor in the rate of theB non-conservation, above which the anomalous processes are certainly in equilibrium after the electroweak phase transition. Assuming that the temperature-dependence of the sphaleron energy is given by that found from the one-loop finitetemperature effective potential, this critical Higgs mass is lowered to a value of the order of 50 GeV.     

暗能量和重子数等曲率扰动

文章对作为暗能量候选者之一的Quintessence场与物质的相互作用及其在宇宙学中的应用进行了研究,通过引入Quintessence与重子流的耦合合理地解释了重子与反重子的不对称性.另外还详细地计算了重子数等曲率扰动.     

Cosmic Strings in Realistic Particle Physics Theories and Baryogenesis

Grand unified theories can admit cosmic stringswith fermion zero modes. Such zero modes result in thestring being current-carrying and the formation ofstable remnants, vortons. However, the string zero modes do not automatically survive subsequentphase transitions. In this case the vortons dissipate.It is possible that the dissipating cosmic vortonscreate the observed baryon asymmetry of the universe. We show that fermion zero modes are anautomatic consequence cosmic strings in supersymmetrictheories. Since supersymmetry is not observed in nature,we consider possible supersymmetry-breaking terms. Some of these terms result in the zero modesbeing destroyed. We calculate the baryon asymmetrygenerated by the consequent dissipating cosmic vortons.If the supersymmetry-breaking scale is high enough, then the dissipating cosmic vortons couldaccount for the observed baryon asymmetry.     

On some properties of the neutron in the statistical model

Using the statistical model to arrive at |ψ(r)|² the square modulus of theS state wavefunction of the neutron, the electric dipole moment |d _n ^e | of the neutron as well as its baryon number violating lifetime have been estimated. The baryon asymmetry of the universe depending on |d _n ^e | has also been studied in this context.     

Bubble collisions in the cosmological quark-hadron phase transition

Assuming that a first-order QCD phase transition occured in the very early universe, we investigate the growth and collisions of hadron bubbles in the thin-wall approximation. We also discuss a mechanism of baryon number concentration.