Violation of<i>CP</i>in variance,<i>C</i>asymmetry, and baryon asymmetry of the universe

Sakharov, Andrej Dmitrievich

doi:10.1070/pu1991v034n05abeh002497

Cited by 1,212 publications

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“…so by using the first decoupling time t D1 (19), the termṘ as a function of the decoupling temperature iṡ…”

Section: Gravitational Baryogenesis In Dgp Brane Cosmologymentioning

confidence: 99%

“…The cosmic microwave background observations [15] and also the Big Bang nucleosynthesis [16] admit this imbalance of matter (baryons) and antimatter (antibaryons). According to the Sakharov benchmark [17][18][19][20], the GB procedure is based on the presence of a CPviolating interaction term so that it can explain the fundamental conditions for the generation of the imbalance of matter and antimatter in the observed universe. In this paper we try to consider the GB process in the context of DGP brane cosmology, and the goal of the present paper is to highlight the differences of the GB process between the DGP brane cosmology and standard cosmology.…”

Section: Introductionmentioning

confidence: 99%

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Gravitational baryogenesis in DGP brane cosmology

Atazadeh

2018

Eur. Phys. J. C

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We consider the imbalance of matter and antimatter by using a gravitational baryogenesis mechanism in the background of Dvali-Gabadadze-Porrati (DGP) brane cosmology. By taking into account a flat Friedmann-Lemaître-Robertson-Walker (FLRW) metric in the DGP brane model, we find that for a radiation dominated universe, w = 1/3, the ratio of baryon number density to entropy from the gravitational baryogenesis is not zero, contrary to ordinary general relativity. Also, we study the ratio of baryon number density to entropy against the observational constraints in DGP cosmology.

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“…so by using the first decoupling time t D1 (19), the termṘ as a function of the decoupling temperature iṡ…”

Section: Gravitational Baryogenesis In Dgp Brane Cosmologymentioning

confidence: 99%

Section: Introductionmentioning

confidence: 99%

Gravitational baryogenesis in DGP brane cosmology

Atazadeh

2018

Eur. Phys. J. C

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“…Until now, in spite of continuing efforts, there is no experimental indication for the existence of such decays, and it was possible only to establish a lower boundary: the lifetime of the proton is longer than 10 34 years. The proton decay could be a missing ingredient for the understanding of the above-mentioned baryonic asymmetry of the Universe (absence of antimatter); other ingredients are violation of  symmetry (combined charge conjugation , transforming particles into antiparticles, and spatial inversion ) and a nonstationary situation that was present at the early stages of the expanding Universe [5]. Other ideas of explaining the matter-antimatter asymmetry of the Universe are related to neutrino physics.…”

Section: Neutron Decaymentioning

confidence: 99%

Building Blocks and Interactions

2017

Physics of Atomic Nuclei

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The standard textbook statement reads "Nuclei consist of protons and neutrons." For the major part of what we are going to discuss in the course, this simple notion is approximately true. Indeed, complex nuclei in the Universe were mostly "cooked" in stars by the processes of consecutive addition of neutrons and protons and their mutual transformations. It is relatively easy to extract these particles back from the nuclei since the separation energy per particle is typically only 6-8 MeV, less than 1% of the mass of the proton (p) or neutron (n) that is of order ∼ 1 GeV = 10 3 MeV.In many nuclei with an abnormal ratio between the proton and neutron numbers, the separation energy is even significantly lower than the value mentioned earlier. And still the statement of our first sentence has a limited range of validity. In general, the answer to the question of nuclear constituents depends on the kind of phenomena we are interested in. Various experimental studies emphasize different aspects of nuclear structure. Different patterns can be resolved at different energy scales by specifically adjusted experimental tools.The nuclear forces that keep the nucleus together are induced through exchange by mediating quanta -mesons, similar to how the electromagnetic interactions are generated by the exchange of photons. Roughly speaking, at energies small compared to the masses of particles that are capable of serving as mediators of nuclear forces, the nucleus indeed looks as an object composed of protons and neutrons. (Note that such a range of energies does not exist in the case of electromagnetic interactions carried by massless photons.) Protons and neutrons have very similar nuclear properties, and they are called by a unifying term "nucleons" (N). The mesons of the lightest family, pions ( +,0,− ), are approximately seven times lighter than the nucleons. Corresponding energies E < m c 2 ≈ 140 MeV define a domain of low-energy nuclear physics where the nucleus can be considered as being made of nonrelativistic nucleons. In this domain, mesons are virtual particles hidden in nucleon-nucleon interactions, and they rarely appear Physics of Atomic Nuclei, First Edition. Vladimir Zelevinsky and Alexander Volya.

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“…Matter and anti-matter particles annihilate. However, because of baryon non-conservation and non-equilibrium conditions described by Sakharov ( 1967 ) , there was a slight excess of baryons over anti-baryons (Dolgov, 1997 ;Quinn and Nir, 2008 ) . If there were not, all of the matter and anti-matter dumped into the universe at reheating would have annihilated and turned into radiation.…”

Section: In Fl Ation Baryon Non-conservation and The Homogeneous DImentioning

confidence: 99%