scholarly journals New Evidence of the Azimuthal Alignment of Quasars Spin Vector in the LQG U1.28, U1.27, U1.11, Cosmologically Explained

2021 ◽  
Author(s):  
Reinoud Jan Slagter
Keyword(s):  
Symmetry Breaking ◽  
Gauge Field ◽  
Cosmic Strings ◽  
Azimuthal Angle ◽  
Polar Angle ◽  
Position Angle ◽  
Radio Spectrum ◽  
Host Galaxy ◽  
Axially Symmetry ◽  
Superconducting Vortices

There has been observational evidence about spin axes of quasars in large quasar groups correlated over hundreds of Mpc. This is seen in the radio spectrum as well as in the optical range. There is not yet a satisfactory explanation of this "spooky" alignment. This alignment cannot be explained by mutual interaction at the time that quasars manifest themselves optically. A cosmological explanation could be possible in the formation of superconducting vortices (cosmic strings) in the early universe, just after the symmetry-breaking phase of the universe. We gathered from the NASA/IPAC and SIMBAD extragalactic databases the right ascension, declination, inclination, position angle and eccentricity of the host galaxies of 3 large quasar groups to obtain the azimuthal and polar angle of the spin vectors. The alignment of the azimuthal angle of the spin vectors of quasars in their host galaxy is confirmed in the large quasar group U1.27 and compared with two other groups in the vicinity, i.e., U1.11 and U1.28. It is well possible that the azimuthal angle alignment fits the predicted azimuthal angle dependency in the theoretical model of the formation of general relativistic superconducting vortices, where the initial axially symmetry is broken just after the symmetry breaking of the scalar-gauge field.} \keyword{quasar groups; alignment spin vectors; host galaxy; cosmic strings; symmetry breaking; scalar-gauge field.

scholarly journals On the azimuthal alignment of quasars spin vector in large quasar groups and cosmic strings

2020 ◽  
Author(s):  
Reinoud J Slagter ◽  
Pieter G Miedema
Keyword(s):  
Symmetry Breaking ◽  
Gauge Field ◽  
Early Universe ◽  
Cosmic Strings ◽  
Azimuthal Angle ◽  
Red Shift ◽  
Host Galaxy ◽  
Spin Vector

Abstract We find evidence of the alignment of the azimuthal angle of the spin vectors of quasars in their host galaxy in large quasar groups of different redshift. This effect could be explained by symmetry breaking of the scalar-gauge field of cosmic strings in the early universe. It is expected that this effect will be more profound for higher red shift.

scholarly journals Evidence of cosmic strings by the observation of the alignment of quasar polarization axes on Mpc scale

2018 ◽  
Vol 27 (09) ◽  
pp. 1850094 ◽  
Author(s):  
Reinoud Jan Slagter
Keyword(s):  
Symmetry Breaking ◽  
Gauge Field ◽  
Cosmic String ◽  
Axial Symmetry ◽  
Approximation Scheme ◽  
Azimuthal Angle ◽  
Goldstone Boson ◽  
Second Order ◽  
Compact Objects ◽  
Warp Factor

The recently found alignment of the polarization axes (PA) of quasars in large quasar groups (LQGs) on Mpc scales can be explained by general relativistic cosmic string networks. By considering the cosmic string as a result of spontaneous symmetry breaking of the gauged U(1) abelian Higgs model with topological charge [Formula: see text], many stability features of [Formula: see text]-vortex solutions of superconductivity can be taken over. Decay of the high multiplicity ([Formula: see text]) super-conducting vortex into a lattice of [Formula: see text] vortices of unit magnetic flux is energetically favorable. The temporarily broken axial symmetry will leave an imprint of a preferred azimuthal-angle on the lattice. The stability of the lattice depends critically on the parameters of the model, especially when gravity comes into play. In order to handle the strong nonlinear behavior of the time-dependent coupled field equations of gravity and the scalar-gauge field, we will use a high-frequency approximation scheme to second order on a warped 5D axially symmetric spacetime with the scalar-gauge field residing on the brane. We consider different winding numbers for the subsequent orders of perturbations of the scalar field. A profound contribution to the energy–momentum tensor comes from the bulk spacetime and can be understood as “dark”-energy. The cosmic string becomes super-massive by the contribution of the 5D Weyl tensor on the brane and the stored azimuthal preferences will not fade away. During the recovery to axial symmetry, gravitational and electro-magnetic radiation will be released. The perturbative appearance of a nonzero energy–momentum component [Formula: see text] can be compared with the phenomenon of bifurcation along the Maclaurin–Jacobi sequence of equilibrium ellipsoids of self-gravitating compact objects, signaling the onset of secular instabilities. There is a kind of similarity with the Goldstone-boson modes of spontaneously broken symmetries of continuous groups. The recovery of the SO(2) symmetry from the equatorial eccentricity takes place on a time-scale comparable with the emission of gravitational waves. The emergent azimuthal-angle dependency in our model can be used to explain the aligned PA in LQGs on Mpc scales. Spin axis direction perpendicular to the major axes of LQGs when the richness decreases can be explained as a second-order effect in our approximation scheme by the higher multiplicity terms. The preferred directions are modulo [Formula: see text], with [Formula: see text] being an integer dependent on the [Formula: see text]th order of approximation. When more data of quasars of high redshift becomes available, one could prove that the alignment emerged after the symmetry breaking scale and must have a cosmological origin. The effect of the warp factor on the second-order perturbations could also be an indication of the existence of extra large dimensions.

scholarly journals Primordial monopoles and strings, inflation, and gravity waves

2021 ◽  
Vol 2021 (2) ◽  
Author(s):  
Joydeep Chakrabortty ◽  
George Lazarides ◽  
Rinku Maji ◽  
Qaisar Shafi
Keyword(s):  
Symmetry Breaking ◽  
Gravity Waves ◽  
Cosmic Strings ◽  
Wave Spectrum ◽  
Gauge Coupling ◽  
String Tension ◽  
Magnetic Monopoles ◽  
Intermediate Scale ◽  
Tension Parameter ◽  
The Universe

Abstract We consider magnetic monopoles and strings that appear in non-supersymmetric SO(10) and E6 grand unified models paying attention to gauge coupling unification and proton decay in a variety of symmetry breaking schemes. The dimensionless string tension parameter Gμ spans the range 10−6− 10−30, where G is Newton’s constant and μ is the string tension. We show how intermediate scale monopoles with mass ∼ 1013− 1014 GeV and flux ≲ 2.8 × 10−16 cm−2s−1sr−1, and cosmic strings with Gμ ∼ 10−11− 10−10 survive inflation and are present in the universe at an observable level. We estimate the gravity wave spectrum emitted from cosmic strings taking into account inflation driven by a Coleman-Weinberg potential. The tensor-to-scalar ratio r lies between 0.06 and 0.003 depending on the details of the inflationary scenario.

scholarly journals A discussion on supersymmetric cosmic strings with gauge-field mixing

2004 ◽  
Vol 6 ◽  
pp. 58-58 ◽  
Author(s):  
C N Ferreira ◽  
C F Godinho ◽  
J A Helayel-Neto
Keyword(s):  
Gauge Field ◽  
Cosmic Strings

scholarly journals Angle deficit and nonlocal gravitoelectromagnetism around a slowly spinning cosmic string

2020 ◽  
Vol 29 (14) ◽  
pp. 2043027
Author(s):  
Jens Boos
Keyword(s):  
Gravitational Field ◽  
Symmetry Breaking ◽  
Early Universe ◽  
Physical Interpretation ◽  
Cosmic String ◽  
Cosmic Strings ◽  
Radial Distance ◽  
Gravitomagnetic Field ◽  
Simply Connected

Cosmic strings, as remnants of the symmetry breaking phase in the Early universe, may be susceptible to nonlocal physics. Here, we show that the presence of a Poincaré-invariant nonlocality—parametrized by a factor [Formula: see text]—regularizes the gravitational field and thereby changes the properties of spacetime: it is now simply connected and the angle deficit around the cosmic string becomes a function of the radial distance. Similar changes occur for the nonlocal gravitomagnetic field of a rotating cosmic string, and we translate these mathematical facts into the language of nonlocal gravitoelectromagnetism and thereby provide a physical interpretation. We hope that these insights might provide a helpful perspective in the search for traces of nonlocal physics in our universe.

Sound radiation from a cylindrical duct. Part 1. Ray structure of the duct modes and of the external field

1994 ◽  
Vol 281 ◽  
pp. 293-311 ◽  
Author(s):  
C. J. Chapman
Keyword(s):  
Piecewise Linear ◽  
Azimuthal Angle ◽  
Polar Angle ◽  
Directivity Pattern ◽  
Acoustic Mode ◽  
Inhomogeneous Waves ◽  
Alternative Description ◽  
Geometrical Theory Of Diffraction ◽  
Pass Through ◽  
Cylindrical Duct

This paper determines the ray structure of a spinning acoustic mode propagating inside a semi-infinite circular cylindrical duct, and thereby determines the ray structure of the field radiated from the end of the duct. Inside the duct, but outside of a caustic cylindrical surface, the rays are piecewise linear helices; on striking the rim of the end-face of the duct, these rays produce ‘Keller cones’ of diffracted rays. The cones determine the structure of the radiated field: for example, no rays penetrate two cone-shaped far-field quiet zones centred on the duct axis; two rays pass through each point in a forward loud zone; and one ray passes through each point in a rearward loud zone. The two rays through each point in the forward loud zone interfere to produce an oscillatory directivity pattern. One quarter of the rays on each cone point back inside the duct and produce the reflected field. Thus the rim of the end-face of the duct acts as a ‘ring source’, in which the radiated and reflected fields have their origin. Every propagating duct mode determines a polar angle and an azimuthal angle; these are taken as parameters specifying the mode and are used to calculate the positions and angles of all the rays. The mathematical method on which the paper is based is Debye's approximation for the Bessel function which appears in the expression for the duct modes; the approximation shows also that the duct contains a region of smooth helical rays on which the field consists of inhomogeneous waves: this region is the inner cylinder, lying inside the annulus of piecewise linear helical rays. The results of the paper are very promising for the application of Keller's geometrical theory of diffraction to detailed calculations of the sound radiated from aeroengine ducts. An alternative description of the field, using Cargill's meridional rays, is summarized.

EXACT WAVE FUNCTIONS AND ENERGIES OF A NON-RELATIVISTIC FREE QUANTUM PARTICLE ON THE SURFACE OF A DEGENERATE TORUS

2004 ◽  
Vol 19 (23) ◽  
pp. 1759-1766 ◽  
Author(s):  
AXEL SCHULZE-HALBERG
Keyword(s):  
Schrödinger Equation ◽  
Closed Form ◽  
Schrodinger Equation ◽  
Quantum Particle ◽  
Azimuthal Angle ◽  
Polar Angle ◽  
Wave Functions ◽  
Exactly Solvable

We study the non-relativistic Schrödinger equation for a free quantum particle constrained to the surface of a degenerate torus, parametrized by its polar and azimuthal angle. On restricting to wave functions that depend on the polar angle only, the Schrödinger equation becomes exactly-solvable. We compute its physical solutions (continuous, normalizable and 2π-periodic) and the associated energies in closed form.

3D ACOUSTIC ANALYSIS OF SPHERICAL CHAMBER HAVING SINGLE INLET AND MULTIPLE OUTLET: AN IMPEDANCE MATRIX APPROACH

2011 ◽  
Vol 03 (04) ◽  
pp. 685-710 ◽  
Author(s):  
A. MIMANI ◽  
M. L. MUNJAL
Keyword(s):  
Bessel Functions ◽  
Acoustic Analysis ◽  
Transmission Loss ◽  
Azimuthal Angle ◽  
Polar Angle ◽  
Impedance Matrix ◽  
Modal Expansion ◽  
3D Fea ◽  
Axisymmetric Shape ◽  
Good Agreement

The transmission loss (TL) performance of spherical chambers having single inlet and multiple outlet is obtained analytically through modal expansion of acoustic field inside the spherical cavity in terms of the spherical Bessel functions and Legendre polynomials. The uniform piston driven model based upon the impedance [Z] matrix is used to characterize the multi-port spherical chamber. It is shown analytically that the [Z] parameters are independent of the azimuthal angle (φ) due to the axisymmetric shape of the sphere; rather, they depend only upon the polar angle (θ) and radius of the chamber R0. Thus, the effects of relative polar angular location of the ports and number of outlet ports are investigated. The analytical results are shown to be in good agreement with the 3D FEA results, thereby validating the procedure suggested in this work.

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