scholarly journals Large-scale magnetic fields can explain the baryon asymmetry of the Universe

2016 ◽  
Vol 93 (8) ◽  
Author(s):  
Tomohiro Fujita ◽  
Kohei Kamada
Keyword(s):  
Magnetic Fields ◽  
Large Scale ◽  
Baryon Asymmetry ◽  
The Universe

scholarly journals Magnetism in the Early Universe

2018 ◽  
Vol 14 (A30) ◽  
pp. 295-298
Author(s):  
Tina Kahniashvili ◽  
Axel Brandenburg ◽  
Arthur Kosowsky ◽  
Sayan Mandal ◽  
Alberto Roper Pol
Keyword(s):  
Magnetic Field ◽  
Magnetic Fields ◽  
Gravitational Waves ◽  
Early Universe ◽  
Large Scale ◽  
Direct Detection ◽  
Correlation Lengths ◽  
Cosmological Scenario ◽  
Expansion Of The Universe ◽  
The Universe

AbstractBlazar observations point toward the possible presence of magnetic fields over intergalactic scales of the order of up to ∼1 Mpc, with strengths of at least ∼10−16 G. Understanding the origin of these large-scale magnetic fields is a challenge for modern astrophysics. Here we discuss the cosmological scenario, focussing on the following questions: (i) How and when was this magnetic field generated? (ii) How does it evolve during the expansion of the universe? (iii) Are the amplitude and statistical properties of this field such that they can explain the strengths and correlation lengths of observed magnetic fields? We also discuss the possibility of observing primordial turbulence through direct detection of stochastic gravitational waves in the mHz range accessible to LISA.

scholarly journals Magnetic fields in the early Universe

2008 ◽  
Vol 4 (S259) ◽  
pp. 529-538 ◽  
Author(s):  
Eduardo Battaner ◽  
Estrella Florido
Keyword(s):  
Phase Transitions ◽  
Magnetic Fields ◽  
Early Universe ◽  
Galaxy Formation ◽  
Faraday Rotation ◽  
Large Scale ◽  
Large Scale Structure ◽  
Anisotropy Spectra ◽  
The Universe ◽  
Negligible Influence

AbstractThere is increasing evidence that intense magnetic fields exist at large redshifts. They could arise after galaxy formation or in very early processes, such as inflation or cosmological phase transitions, or both. Early co-moving magnetic strengths in the range 1-10 nG could be present at recombination. The possibilities to detect them in future CMB experiments are discussed, mainly considering their impact in the anisotropy spectra as a result of Faraday rotation and Alfven waves. Magnetic fields this magnitude could also have a non-negligible influence in determining the filamentary large scale structure of the Universe.

scholarly journals Relativistic plasma and ICM/radio source interaction

2010 ◽  
Vol 6 (S274) ◽  
pp. 340-347 ◽  
Author(s):  
Luigina Feretti ◽  
Gabriele Giovannini ◽  
Federica Govoni ◽  
Matteo Murgia
Keyword(s):  
Magnetic Fields ◽  
Radio Source ◽  
Large Scale ◽  
Large Scale Structure ◽  
Radio Sources ◽  
Relativistic Electrons ◽  
Coma Cluster ◽  
Cluster Of Galaxies ◽  
Formation And Evolution ◽  
The Universe

AbstractThe first detection of a diffuse radio source in a cluster of galaxies, dates back to the 1959 (Coma Cluster, Large et al. 1959). Since then, synchrotron radiating radio sources have been found in several clusters, and represent an important cluster component which is linked to the thermal gas. Such sources indicate the existence of large scale magnetic fields and of a population of relativistic electrons in the cluster volume. The observational results provide evidence that these phenomena are related to turbulence and shock-structures in the intergalactic medium, thus playing a major role in the evolution of the large scale structure in the Universe. The interaction between radio sources and cluster gas is well established in particular at the center of cooling core clusters, where feedback from AGN is a necessary ingredient to adequately describe the formation and evolution of galaxies and host clusters.

BARYOGENESIS IN THE INFLATIONARY UNIVERSE —THE INSTANTANEOUS REHEATING MODEL—

1987 ◽  
Vol 02 (06) ◽  
pp. 1809-1828 ◽  
Author(s):  
JUN’ICHI YOKOYAMA ◽  
HIDEO KODAMA ◽  
KATSUHIKO SATO ◽  
NOBUAKI SATO
Keyword(s):  
Thermal Equilibrium ◽  
Large Scale ◽  
Baryon Asymmetry ◽  
Higgs Bosons ◽  
Boson Mass ◽  
Inflationary Universe ◽  
Higgs Boson Mass ◽  
Boltzmann Equations ◽  
Thermal Equilibrium State ◽  
The Universe

Baryogenesis in the inflationary universe is investigated, assuming that the universe is reheated instantaneously. Boltzmann equations are numerically integrated to trace time evolution of asymmetries in quarks and leptons in the Friedmann stage after the reheating, starting from the thermal equilibrium state. It is shown that the sign of the final baryon asymmetry may change depending on the reheating temperature as a result of interplay of superheavy gauge and Higgs bosons, and its mechanism is clarified. Furthermore we suggest a mechanism of generating isocurvature fluctuations which could be the origin of the large scale structure of the universe. It is also found in the instantaneous reheating model that the reheating temperature Ti must satisfy Ti>MH/10 (MH: Higgs boson mass) for the observed baryon/entropy ratio to be explained.

scholarly journals From the Early Universe to the Modern Universe

Symmetry ◽  
2020 ◽  
Vol 12 (3) ◽  
pp. 382
Author(s):  
V. V. Burdyuzha
Keyword(s):  
Dark Matter ◽  
Dark Energy ◽  
Large Scale ◽  
Cosmological Solution ◽  
Baryon Asymmetry ◽  
Composite Model ◽  
Quantum Process ◽  
Goldstone Bosons ◽  
The Universe ◽  
Relativistic Phase

The birth of the Universe, its dark components, and the next fundamental level of matter are briefly discussed. The classical cosmological solution for our Universe with a Λ-term has two branches divided by a gap. The quantum process of tunneling between branches took place. A model of a slowly swelling Universe in the result of the multiple reproductions of cosmological cycles arises naturally. The occurrence of baryon asymmetry is briefly discussed. The problem of the cosmological constant is solved and, thus, the crisis of physics connected with this constant is overcome. But we note that dark energy is evolving. Dark matter (part or all) consists of familon-type pseudo-Goldstone bosons with a mass of 10−5–10−3 eV. It follows the composite model of particles. This model reproduces three relativistic phase transitions in the medium of familons at different red shifts, forming a large scale structure of the Universe dark matter that was “repeated” by baryons. Here three generations of elementary particles are absolutely necessary.

scholarly journals Magnetic Fields in the Large-Scale Structure of the Universe

2011 ◽  
Vol 166 (1-4) ◽  
pp. 1-35 ◽  
Author(s):  
D. Ryu ◽  
D. R. G. Schleicher ◽  
R. A. Treumann ◽  
C. G. Tsagas ◽  
L. M. Widrow
Keyword(s):  
Magnetic Fields ◽  
Large Scale ◽  
Large Scale Structure ◽  
Scale Structure ◽  
The Universe

scholarly journals Turbulence and Magnetic Fields in the Large-Scale Structure of the Universe

Science ◽  
2008 ◽  
Vol 320 (5878) ◽  
pp. 909-912 ◽  
Author(s):  
D. Ryu ◽  
H. Kang ◽  
J. Cho ◽  
S. Das
Keyword(s):  
Magnetic Fields ◽  
Large Scale ◽  
Large Scale Structure ◽  
Scale Structure ◽  
The Universe

GENERATION OF LARGE-SCALE MAGNETIC FIELDS FROM PRIMORDIAL DENSITY FLUCTUATIONS

2007 ◽  
Vol 22 (25n28) ◽  
pp. 2091-2098 ◽  
Author(s):  
KIYOTOMO ICHIKI ◽  
KEITARO TAKAHASHI ◽  
NAOSHI SUGIYAMA ◽  
HIDEKAZU HANAYAMA ◽  
HIROSHI OHNO
Keyword(s):  
Magnetic Fields ◽  
Electric Fields ◽  
Large Scale ◽  
Density Fluctuations ◽  
Light Elements ◽  
Cosmological Recombination ◽  
Primordial Plasma ◽  
Wide Range ◽  
Density Perturbations ◽  
The Universe

We investigate a generation of magnetic fields from cosmological density perturbations. In the primordial plasma before cosmological recombination, all of the materials except dark matter in the universe exist in the form of photons, electrons, and protons (and a small number of light elements). Due to the different scattering nature of photons off electrons and protons, electric currents and electric fields are inevitably induced, and thus magnetic fields are generated. We numerically obtain the power spectrum of magnetic fields over a wide range of scales, from k ~ 10−5 Mpc −1 to k ~ 109 Mpc −1. Implications of these cosmologically generated magnetic fields are discussed.

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