553 research outputs found
Cosmology and New Physics
A comparison of the standard models in particle physics and in cosmology
demonstrates that they are not compatible, though both are well established.
Basics of modern cosmology are briefly reviewed. It is argued that the
measurements of the main cosmological parameters are achieved through many
independent physical phenomena and this minimizes possible interpretation
errors. It is shown that astronomy demands new physics beyond the frameworks of
the (minimal) standard model in particle physics. More revolutionary
modifications of the basic principles of the theory are also discussed.Comment: 37 pages, 5 figures; lectures presented at 9th International Moscow
School of Physics (34th ITEP Winter School
In-Plane Spectral Weight Shift of Charge Carriers in
The temperature dependent redistribution of the spectral weight of the
plane derived conduction band of the high
temperature superconductor (T_c = 92.7 K) was studied with wide-band (from 0.01
to 5.6 eV) spectroscopic ellipsometry. A superconductivity - induced transfer
of the spectral weight involving a high energy scale in excess of 1 eV was
observed. Correspondingly, the charge carrier spectral weight was shown to
decrease in the superconducting state. The ellipsometric data also provide
detailed information about the evolution of the optical self-energy in the
normal and superconducting states
Plane-Symmetric Inhomogeneous Bulk Viscous Cosmological Models with Variable
A plane-symmetric non-static cosmological model representing a bulk viscous
fluid distribution has been obtained which is inhomogeneous and anisotropic and
a particular case of which is gravitationally radiative. Without assuming any
{\it adhoc} law, we obtain a cosmological constant as a decreasing function of
time. The physical and geometric features of the models are also discussed.Comment: 11 page
Calculation of Nucleon Electromagnetic Form Factors
The fomalism is developed to express nucleon matrix elements of the
electromagnetic current in terms of form factors consistent with the
translational, rotational, and parity symmetries of a cubic lattice. We
calculate the number of these form factors and show how appropriate linear
combinations approach the continuum limit.Comment: Lattice 2002 (hadronic matrix elements) 3 page
On the T-dependence of the magnetic penetration depth in unconventional superconductors at low temperatures: can it be linear?
We present a thermodynamics argument against a strictly linear temperature
dependence of the magnetic penetration depth, which applies to superconductors
with arbitrary pairing symmetry at low temperatures.Comment: 5 pages, expanded version of cond-mat/971102
Bianchi Type I Magnetofluid Cosmological Models with Variable Cosmological Constant Revisited
The behaviour of magnetic field in anisotropic Bianchi type I cosmological
model for bulk viscous distribution is investigated. The distribution consists
of an electrically neutral viscous fluid with an infinite electrical
conductivity. It is assumed that the component of shear tensor
is proportional to expansion () and the coefficient of
bulk viscosity is assumed to be a power function of mass density. Some physical
and geometrical aspects of the models are also discussed in presence and also
in absence of the magnetic field.Comment: 13 page
Ellipsoidal Universe Can Solve The CMB Quadrupole Problem
The recent three-year WMAP data have confirmed the anomaly concerning the low
quadrupole amplitude compared to the best-fit \Lambda CDM prediction. We show
that, allowing the large-scale spatial geometry of our universe to be
plane-symmetric with eccentricity at decoupling or order 10^{-2}, the
quadrupole amplitude can be drastically reduced without affecting higher
multipoles of the angular power spectrum of the temperature anisotropy.Comment: 4 pages, 2 figures, minor changes, reference added, to appear in
Phys. Rev. Let
Quantum Evolution of the Bianchi Type I Model
The behaviour of the flat anisotropic model of the Universe with a scalar
field is explored within the framework of quantum cosmology. The principal
moment of the account of an anisotropy is the presence either negative
potential barrier or positive repelling wall. In the first case occur the above
barrier reflection of the wave function of the Universe, in the second one
there is bounce off a potential wall. The further evolution of the Universe
represents an exponential inflating with fast losses of an anisotropy and
approach to the standard cosmological scenario.Comment: Latex, 18 pages, 5 figure
Fermi Surface Nesting and the Origin of the Charge Density Wave in NbSe
We use highly accurate density functional calculations to study the band
structure and Fermi surfaces of NbSe2. We calculate the real part of the
non-interacting susceptibility, Re chi_0(q), which is the relevant quantity for
a charge density wave (CDW) instability and the imaginary part, Im chi_0(q),
which directly shows Fermi surface (FS) nesting. We show that there are very
weak peaks in Re chi_0(q) near the CDW wave vector, but that no such peaks are
visible in Im chi_0(q), definitively eliminating FS nesting as a factor in CDW
formation. Because the peak in Re chi_0(q) is broad and shallow, it is unlikely
to be the direct cause of the CDW instability. We briefly address the
possibility that electron-electron interactions (local field effects) produce
additional structure in the total (renormalized) susceptibility, and we discuss
the role of electron-ion matrix elements.Comment: Replacement of Table II values, minor changes to tex
Big Bang Nucleosynthesis Constraints on Primordial Magnetic Fields
We reanalyze the effect of magnetic fields in BBN, incorporating several
features which were omitted in previous analyses. We find that the effects of
coherent magnetic fields on the weak interaction rates and the electron
thermodynamic functions (\rhoe, \Pe, and \drhoedt ) are unimportant in
comparison to the contribution of the magnetic field energy density in BBN. In
consequence the effect of including magnetic fields in BBN is well approximated
numerically by treating the additional energy density as effective neutrino
number. A conservative upper bound on the primordial magnetic field,
parameterized as , is (). This bound can be stronger than the conventional bound coming from
the Faraday rotation measures of distant quasars if the cosmological magnetic
field is generated by a causal mechanism.Comment: Latex, 20 pages, 3 uuencoded figures appende
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