arXiv subjects
Publications and source records attributed to Leonard S. Kisslinger.
Using the QCD Sum Rule Method, we estimate the mass of the lowest strange hybrid baryon with $IJ^P=0(1/2)^-$. We find the mass is approximately that of the $Λ(1405)$, whose nature has been a puzzle for many decades. Possible tests of this result are discussed.
The non-local vacuum condensates of QCD describe the distributions of quarks and gluons in the non-perturbative QCD vacuum. Physically, this means that vacuum quarks and gluons have nonzero mean-squared momentum, called virtuality. In this paper we study the quark virtuality which is given by the ratio of the local quark-gluon mixed vacuum condensate to the quark local vacuum condensate. The two vacuum condensates are obtained by solving Dyson-Schwinger Equations of a fully dressed quark propagator with an effective gluon propagator. Using our calculated condensates, we obtain the virtuality of quarks in the QCD vacuum state. Our numerical predictions differ from the other theoretical model calculations such as QCD sum rules, Lattice QCD and instanton models.
Using EW-MSSM field theory, so the EWPT is first order, we derive the equations of motion for the gauge fields. With an isospin ansatz we derive e.o.m. for the electrically charged W fields uncoupled from all other fields. These and the lepton currents serve as the current for the Maxwell-like e.o.m. for the electromagnetic field. The electromagnetic field arising during EWPT bubble nucleation without leptons is found. We then calculate the electron current contribution, which is seen to be quite large. This provides the basis for determinining the magnetic field created by EWPT bubble collisions, which could seed galactic and extra-galactic magnetic fields.
We investigate the momentum given to a protoneutron star, the pulsar kick, during the first 10 seconds after temperature equilibrium is reached. Using a model with two sterile neutrinos obtained by fits to the MiniBoone and LSND experiments there is a large mixing angle, and the effective volume for emission is calculated. Using formulations with neutrinos created by URCA processes in a strong magnetic field, so the lowest Landau level has a sizable probability, we find that with known paramenters the asymmetric sterile neutrino emissivity might account for large pulsar kicks.
We estimate the energy of the lowest Charmonium and Upsilon states with hybrid admixtures using the method of QCD Sum Rules. Our results show that the $Ψ'(2S)$ and $Υ(3S)$ states both have about a 50% admixture of hybrid and meson components. From this we find explanations of both the famous $ρ-π$ puzzle for Charmonium, and the unusual pattern of $σ$ decays that have been found in $Υ$ decays. Moreover, this picture can be used for predictions of heavy quark production with the octet model for RHIC.
We use a model with two sterile neutrinos obtained by fits to the MiniBoone and LSND experiments. Using formulations with neutrinos created by URCA Processes in a strong magnetic field, so the lowest Landau level has a sizable probability, we find that with known paramenters the assymetric sterile neutrino emissivity might account for large pulsar kicks.
Using the method of QCD Sum Rules, we estimate the energy of the lowest hybrid Charmonium state, and find it to be at the energy of the $Ψ'(2S)$ state, about 600 Mev above the $J/Ψ(1S)$ state. Since our solution is not consistent with a pure hybrid at this energy, we conclude that the $Ψ'(2S)$ state is probably an admixed $c \bar{c}$ and hybrid $c \bar{c}g$ state. From this conjecture we find a possible explanation of the famous $ρ-π$ puzzle.
We derive the equations of motion for electroweak MSSM with a right-handed Stop, from which we derive the equations for the electromagnetic field that arises from bubble nucleation and collisions during the first order electroweak phase transition that can occur in this MSSM. Introducing an isospin ansatz we derive e.o.m. for the electrically charged W fields uncoupled from all other fields. These serve as the current for the Maxwell-like e.o.m. for the em field. The resulting electromagnetic field arising during EWPT bubble nucleation is found. This electromagnetic structure, along with that arising from bubble collisions, could seed galactic and extra-galactic magnetic fields.
We derive the energy asymmetry given the proto-neutron star during the time when the neutrino sphere is near the surface of the proto-neutron star, using the modified URCA process. The electrons produced with the anti-neutrinos are in Landau levels due to the strong magnetic field, and this leads to asymmetry in the neutrino momentum, and a pulsar kick. The magnetic field must be strong enough for a large fraction of the eletrons to be in the lowest Landau level, however, there is no direct dependence of our pulsar velocity on the strength of the magnetic field. Our main prediction is that the large pulsar kicks start at about 10 s and last for about 10 s, with the corresponding neutrinos correlated in the direction of the magnetic field. We predict a pulsar velocity of 1.03 $\times 10^{-4} (T/10^{10}K)^7$ km/s, which reaches 1000 km/s if T $\simeq 9.96 \times 10^{10}$ K.
We calculate the magnetic field generated during bubble collisions in a first-order electroweak phase transition that may occur for some choices of parameters in the minimal supersymmetric Standard Model. We show that for sufficiently gentle collisions, where the Higgs field is relatively unperturbed in the bubble overlap region, the equations of motion can be linearized so that in the absence of fermions the charged W fields are the source of the electromagnetic current for generating the seed fields. Solutions of the equations of motion for the charged gauge fields and Maxwell's equations for the magnetic field in O(1,2) space-time symmetry are expressed in closed form by applying boundary conditions at the time of collision. Our results indicate that the magnetic fields generated by charged $W^{\pm}$ fields in the collision are comparable to those found in previous work. The magnetic fields so produced could seed galactic and extra-galactic magnetic fields observed today.
We derive the energy asymmetry given the proto-neutronstar during the time when the neutrino sphere is near the surface of the proto-neutron star, using the modified URCA process. The electrons produced with the anti-neutrinos are in Landau levels due to the strong magnetic field, and this leads to asymmetry in the neutrino momentum, and a pulsar kick. Our main prediction is that the large pulsar kicks start at about 10 s and last for about 10 s, with the corresponding neutrinos correlated in the direction of the magnetic field.
We include the electromagnetic currents from fermion degrees of freedom in the equations of motion for electroweak MSSM with a right-handed Stop that we have recently investigated. It is found that near the surface of the bubble walls there are important effects on the electromagnetic fields produced during bubble nucleation.
Starting from the QCD Lagrangian and the surface tension of QCD bubbles we derive the critical size of bubbles, the nucleation probability and the nucleation site separation distance. We find the separation of sites is more than an order of magnitude larger than previous QCD model estimates, which could lead to observable effects.
The Pomeron, which dominates high energy elastic and diffractive hadronic processes, must be largely gluonic in nature. We use a recent picture of a scalar glueball/sigma system with coupling of the sigma to glue determined from experiment to predict strong peripheral sigma production in the pp$π^0π^0$ and double sigma production in the pp$π^0π^0π^0π^0$ channels.
After a review of CMBR correlations and recent observations, a study of possible CMBR observations of the QCD early universe phase transition is discussed. A model for the QCD bubble walls gives the surface tension found in lattice calculations, and a 1+1 dimensional treatment in this model for bubble collisions shows an interior gluonic wall, a disk with the thickness of a nucleon and horizon size radius. This could lead to a similar magnetic wall, which would produce B-B type CMBR polarization correlations distinct from very early universe models. The study of magnetic fields produced in bubble collisions in MSSM models with a first order Electroweak Phase Transition is also discussed.
This article on light cone field theory reviews the basic concepts of the Poincare group in light cone quantum mechanics and light cone field theory. It discusses recent progress in light cone representations of the Bethe-Salpeter equation, with application to the pion form factor, and the quark Schwinger-Dyson equation. Applications are discussed for deeply virtual Compton scattering, particularly for skewed parton distributions of the pion, and rare B to lepton pair decays. Meson light cone wave functions and recent experimental studies of light cone wave functions are discussed. This review was motivated by the LANL Light Cone 2002 International Workshop.
We use the method of QCD sum rules to investigate a possible hybrid baryon with the quantum numbers of the $Λ$. Using a current composed of uds quarks in a color octet and a gluon, a strange hybrid, the $Λ_H$ is found about 500 MeV above the $Λ$, and we identify it as the $Λ(1600)$. Using our sigma/glueball model we predict a large branching fraction for the $Λ_H \to Λ+ σ(ππ$ resonance), and the experimental search for this decay mode could provide a test of the hybrid nature of the $/Lambda(1600)$.
Starting from the QCD action in an instanton-like SU(2) Yang-Mills field theory, we derive equations of motion in Minkowski space. Possible bubble collisions are studued in a (1+1)-dimension reduction . We find gluonic structures like interior walls, which might give rise to CMBR effects.