An implementation of estimating the two-to-two K-matrix from finite-volume energies based on the Lüscher formalism and involving a Hermitian matrix known as the "box matrix" is described. The method includes higher partial waves and multiple decay channels. Two fitting procedures for estimating the K-matrix parameters, which properly incorporate all statistical covariances, are discussed. Formulas and software for handling total spins up to S = 2 and orbital angular momenta up to L = 6 are obtained for total momenta in several directions. First tests involving ρ-meson decay to two pions include the L = 3 and L = 5 partial waves, and the contributions from these higher waves are found to be negligible in the elastic energy range.

We use the method of QCD Sum Rules to estimate the masses of the charm baryon, Λ + c , bottom baryon Λ 0 b , strange baryon Λ 0 s and compare them to their experimental values.

The mass-varying neutrino scenario is analyzed for three trial quintessence potentials (Ferreira-Joyce, inverse exponential, and thawing oscillating). The neutrino mass is generated via Yukawa coupling to the scalar field which represents dark energy. The inverse exponential and oscillating potentials are shown to successfully generate the neutrino masses in the range m ∼ 10-2-10-3 eV and to yield the current dark energy density in the regime of the late-time acceleration of the Universe. Depending on the choice of potentials, the acceleration could occur in two different regimes: (1) the regime of instability, and (2) the stable regime. The first regime of instability is after the Universe underwent a first-order transition and is rolling toward the new stable vacuum. The imaginary sound velocity c2 s < 0 in this regime implies growing fluctuations of the neutrino density (clustering). In the second regime, the Universe smoothly changes its stable states via a continuous transition. Since c2 s > 0, the neutrino density is stable. For all cases the predicted late-time acceleration of the Universe is asymptotically very close to that of the ΛCDM model. Further extensions of the theory to modify the neutrino sector of the Standard Model and to incorporate inflation are also discussed. It is also shown that in the stable regimes where the neutrino mass is given by the minimum of the thermodynamic potential, the tree-level dynamics of the scalar field is robust with respect to one-loop bosonic and fermionic corrections to the potential.

This is an extension of our recent work on D + (cd), D o (cū) production from p-p and d-Au collisions to B + (bd), B o (bū) production from p-p and A-A collisions. The rapidity cross sections for B + (cd), B o (bū) production from both p-p and A-A collisions are estimated. Our present work makes use of previous work on J/Ψ, Ψ ′ (2S), Υ(nS) production in p-p and A-A collisions, with the main new aspect being the fragmentation probability, D b→bq , which turns out to be similar to the fragmentation probability D c→cq used in our recent work.

We estimate the gravitational wave amplitude as a function of frequency produced during the creation of pulsars from the gravitational collapse of a massive star. The three main quantities needed are the magnitude of the magnetic field producing pulsar kicks, the temperature which determines the velocity of the pulsar and the duration time for the gravitational radiation.