The Production of Magnetic Monopoles in the Very Early Universe

1980 ◽  
pp. 569-582 ◽  
Author(s):  
Martin B. Einhorn
Keyword(s):  
Early Universe ◽  
Magnetic Monopoles

MONOPOLE ACCRETION BY COSMIC STRINGS

1990 ◽  
Vol 05 (17) ◽  
pp. 1313-1320
Author(s):  
A.M. MATHESON ◽  
D.M. UPTON
Keyword(s):  
Black Holes ◽  
Neutron Star ◽  
Early Universe ◽  
Cosmic String ◽  
Cosmic Strings ◽  
Magnetic Monopoles ◽  
Accretion Process

We study the accretion of super-heavy magnetic monopoles around cosmic string loops in the very early universe. For sufficiently massive monopoles, a possible result of this accretion process is the formation of monopole-black holes, leading ultimately to a monopole-to-photon ratio comparable to the limits required by neutron star observations.

Magnetic Monopoles in the Early Universe: Pair Production

Astrophysics ◽  
2003 ◽  
Vol 46 (4) ◽  
pp. 422-428 ◽  
Author(s):  
V. K. Dubrovich ◽  
N. A. Sushko
Keyword(s):  
Pair Production ◽  
Early Universe ◽  
Magnetic Monopoles

MODEL FOR EFFICIENT MONOPOLE ANNIHILATION AND BARYOGENESIS

1995 ◽  
Vol 10 (03) ◽  
pp. 227-233 ◽  
Author(s):  
SUBIR MOHAN
Keyword(s):  
Transition Temperature ◽  
Early Universe ◽  
Higgs Doublet ◽  
Magnetic Monopoles ◽  
Coupling Constants ◽  
Group Symmetry ◽  
Scalar Coupling ◽  
Grand Unification ◽  
Temperature Scales ◽  
The Right

We present a model for efficient annihilation of magnetic monopoles which is accomplished by breaking the electromagnetic gauge invariance for an appropriate range of temperature during the radiation dominated epoch of the early universe. Except for the brief period when electromagnetism is broken, the gauge-group symmetry is SU (3)c × SU (2)L × U (1)Y between the grand unification and electroweak transition temperature scales. The model consists of a standard Higgs doublet, a charged singlet and an uncharged singlet, and it is shown to work for a very general set of parameters with none of the scalar coupling constants being, necessarily, either too large or too small. The uncharged singlet can easily give adequately large Majorana mass to the right-handed neutrinos making baryogenesis possible through the decay of heavy right-handed neutrinos and sphaleron interactions.

The early universe

1989 ◽  
Vol 159 (10) ◽  
pp. 393
Author(s):  
Ya.A. Smorodinskii
Keyword(s):  
Early Universe

Existence of magnetic monopoles in higher dimensions is analogous to unipolar gravity

2020 ◽  
Author(s):  
Deep Bhattacharjee
Keyword(s):  
Flux Density ◽  
Higher Dimensions ◽  
Closed Surface ◽  
Magnetic Monopoles ◽  
Surface Integral ◽  
Flux Tubes ◽  
Spatial Dimensions ◽  
Net Flux ◽  
Field Lines ◽  
The Universe

Gravity has been leaking in higher dimensions in the bulk. Gravity being a closed string is not attached or does not have any endpoints unlike photons to any Dirichlet (p)-Branes and therefore can travel inter-dimensional without any hindrance. In LHC, CERN, Gravitons are difficult to detect as they last for such a short span of time and in most of the cases invisible as because they can escape to higher spatial dimensions to the maximum of 10, as per 'M'-Theory. Gravity being one of the 4-Fundamental forces is weaker than all 3 (strong and weak nuclear force, electromagnetism) and therefore a famous problem has been made in particle physics called the 'hierarchy problem'. Through comprehensive analysis and research I have come to the conclusion that if dimension is 5 (or 4 if we neglect the temporal dimensions) then an old approach is there for the compactification of the dimensions as per Kaluza-Klein theory and the most important implications of this theory is that an unification of electromagnetism with gravitation occurs in the fifth dimensions, therefore we can conclude that both the charge (electric as well as magnetic and gravity) are dependent of each other in case of Dimensions greater than 4 (5 if time is added). Now, basic principles of electromagnetic theory states that the field-flux density through a closed surface like a T 2 Torus when integrated over the surface area leads to a zero flux. That means there is no flux outside this closed surface integral. However, if the surface is open then the field flux density is not zero and this preserves the concept of magnetic monopoles. However, in a paper in 1931,[1] Dirac approaches monopole theory of magnetism through a different perspectives that, if all the electrical charges of the universe is quantized[2] then there is a suitable (not yet proved though) existence of monopoles; however this are not well understood as of today's scenario. In condensed matter physics, plasma physics and magneto hydrodynamics, there are flux tubes and as the both ends of the flux tubes are independent of each other then the net flux through the cylinder is zero as the amount of field lines entering the tube on one side is equal to the amount of field lines exit from the other end. And in the sides of the cylinder or the flux tube there is no escape of field lines, hence, net flux is conserved. There also exists a type of 'Quasiparticles' that can act as a monopole.[3][4][5] Now, from the perspectives of the Guess law of electromagnetism, if there exists a magnetic monopole then the net charge or flux density over a surface is not zero rather the divergence of the flux density B is 4 [6]and an alternative approach of the 'monopole' can be achieved by increasing the spatial dimensions by a factor of 1 or more. The Gravity has no such poles and therefore can be considered as a unipolar flux density existing throughout the universe and is applicable to the inverse square law of decreasing magnitude via distance as 1/r 2. However, a magnet is always of bipolar with a north and South Pole. If a magnet can be broken then also the broken parts develop the other poles and become bipolar. However, there are tiny domains inside a magnet and if a magnet can be heated to approx. 700℃ then all the poles disappeared and if its cooled quickly, rather very quickly then the tiny domains inside the magnet would not get enough time to rearrange themselves and multipolar magnet is developed therefore to preserve the bipolar properties, the magnet should be cooled slowly allowing the time given to the tiny domains top rearrange themselves. Therefore, even multipole can be achieved quite easily but not the monopoles. So, the equation for a closed surface integral of a flux density without monopole is ∯(S) B dS = 0 or ∇ • B = 0 and that closed surface can be considered as 2 types namely (we will discuss about torus) as because in string theory compactification of higher spatial dimensions occurs in torus.

scholarly journals VIBRATIONAL LEVEL POPULATION OF H 2 AND H + 2 IN THE EARLY UNIVERSE

2011 ◽  
Vol 193 (1) ◽  
pp. 7 ◽  
Author(s):  
Carla M. Coppola ◽  
Savino Longo ◽  
Mario Capitelli ◽  
Francesco Palla ◽  
Daniele Galli
Keyword(s):  
Early Universe ◽  
Vibrational Level ◽  
Level Population

scholarly journals IMPLICATIONS OF A QUANTUM MECHANICAL TREATMENT OF THE UNIVERSE

1998 ◽  
Vol 13 (05) ◽  
pp. 347-351 ◽  
Author(s):  
MURAT ÖZER
Keyword(s):  
Quantum Mechanics ◽  
Wave Packet ◽  
Early Universe ◽  
Mechanical Treatment ◽  
Correspondence Principle ◽  
Scale Factor ◽  
Quantum Mechanical ◽  
Quantum Mechanical Treatment ◽  
The Standard Model ◽  
The Universe

We attempt to treat the very early Universe according to quantum mechanics. Identifying the scale factor of the Universe with the width of the wave packet associated with it, we show that there cannot be an initial singularity and that the Universe expands. Invoking the correspondence principle, we obtain the scale factor of the Universe and demonstrate that the causality problem of the standard model is solved.

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