arXiv subjects
Publications and source records attributed to M. Fukugita.
We propose a non-perturbative method to determine the mixing coefficients of $Δs=2$ four-quark operators for the Wilson quark action using chiral Ward identities. The method is applied to calculate B_K in quenched QCD.
We explore the problems in calculating the decay constant for heavy-light mesons using the quenched Wilson quark action for both heavy and light quarks. We find that the continuum limit of the decay constant is reasonably converged among different prescriptions after the continuum limit is taken. A number of technical problems associated with prescriptions are also addressed.
We present new results of our ongoing project toward a precision determination of the kaon $B$ parameter with the Kogut-Susskind quark action in quenched QCD. New results taken at $β$=6.4 and $β=5.7$ suggest that an apparently linear $a$ dependence of $B_K$ previously observed for $β=5.85-6.2$ arises from a change of curvature from convex to concave as the lattice spacing is reduced. Fitting data for $β\geq 5.93$ with an $O(a^2)$ form yields $B_K$(NDR,2 GeV)=0.587(7)(17) in the continuum limit. We also describe a finite-size study of $B_K$ at $β=$ 6.0 and 6.4, and a reanalysis of the theoretical argument for $O(a^2)$ behavior.
A recent observation of Steidel et al. indicates that a substantial fraction of giant galaxies were formed at an epoch as early as redshift $z>3-3.5$. We show that this early formation of giant galaxies gives strong constraints on models of cosmic structure formation. Adopting the COBE normalization for the density perturbation spectrum, we argue that the following models do not have large enough power on galactic scales to yield the observed abundance: (i) standard cold dark matter (CDM) models (where mass density $Ω_0=1$ and power index $n=1$) with the Hubble constant $h\lsim 0.35$; (ii) tilted CDM models with $h=0.5$ and $n\lsim 0.75$; (iii) open CDM models with $h\lsim 0.8$ and $Ω_0 \lsim 0.3$, and (iv) mixed dark matter models with $h=0.5$ and $Ω_ν\gsim 0.2$. Flat CDM models with a cosmological constant $λ_0 \sim 0.7$ are consistent with the observation, provided that $h\gsim 0.6$. Combined with constraints from large-scale structure formation, these results imply that the flat CDM model with a low $Ω_0$ is the only one that is fully consistent with observations. We predict that these high-redshift galaxies are more strongly clustered than normal galaxies observed today.
Assuming that MSW neutrino oscillations occur and ignoring all solar physics except for the constraint that nuclear fusion produces the solar luminosity, we show that new solar neutrino experiments are required to rule out empirically the hypothesis that the sun shines via the CNO cycle.
A lattice QCD calculation of the proton matrix element of the flavor singlet axial-vector current is reported. Both the connected and disconnected contributions are calculated, for the latter employing the variant method of wall source without gauge fixing. From simulations in quenched QCD with the Wilson quark action on a $16^3\times 20$ lattice at $β=5.7$ (the lattice spacing $a\approx 0.14$fm), we find $ΔΣ=Δu+Δd+Δs=+0.638(54)-0.347(46)-0.109(30) = +0.18(10)$ with the disconnected contribution to $Δu$ and $Δd$ equal to $-0.119(44)$, which is reasonably consistent with the experiment.
In the now well established conventional view (see Rees [1] and references therein), quasi-stellar objects (QSOs) and related active galactic nuclei (AGN) phenomena are explained as the result of accretion of plasma onto giant black holes which are postulated to form via gravitational collapse of the high density regions in the centers of massive host galaxies. This model is supported by a wide variety of indirect evidence and seems quite likely to apply at least to some observed AGN phenomena. However, one surprising set of new Hubble Space Telescope (HST) observations [2-4] directly challenges the conventional model, and the well known evolution of the QSO population raises some additional, though not widely recognized, difficulties. We propose here an alternative possibility: the Universe contains a substantial independent population of super-massive black holes, and QSO's are a phenomenon that occurs due to their collisions with galaxies or gas clouds in the intergalactic medium (IGM). This hypothesis would naturally explain why the QSO population declines very rapidly towards low redshift, as well as the new HST data.
Lattice QCD calculation of s-wave hadron scattering lengths in the channels π-π, π-N, K-N, {\bar K}-N and N-N is carried out in the quenched QCD at $β=6/g^2=5.7$. A variant of the method of wall sourceis developed for this purpose, which reduces the computer time by a factor L^3 on an L^3xT lattice compared to the conventional point source method and avoids the Fierz mixing problem. A version of the method in which gauge configurations are not fixed to any gauge can be extended to calculate disconnected quark loop con- tributions in hadron two- and three-point functions. An analytical estimate of statistical errors for this method is worked out, and the magnitude of errors without and with gauge fixing is compared for the case of π-πfour-point functions calculated with the KS quark action. For π-πscattering both I=0 and 2 scattering lengths are evaluated using the KS and Wilson quark actions on a 12^3x20 lattice. For the same size of lattice, π-N, K-N and {\bar K}-N scattering lenghts are calculated with the Wilson quark action. For the π-πand π-N cases simulation results are consistent with the predictions of current algebra and PCAC within one to two standard deviations up to quite heavy quark masses corresponding to $m_π/m_ρ\approx 0.74$, while for the K-N and {\bar K}-N cases the agreement is within a factor of two. For N-N scat- tering simulations with the Wilson action on a 20^4 lattice with heavy quarks with $m_π/m_ρ\approx 0.74-0.95$, where the deuteron is expected to become unbound from a phenomenological study with one-boson exchange potentials, show that the nucleon-nucleon force is attractive for both spin triplet and singlet channels, and that the scattering lengths are substantially larger compared to those for the π-πand π-N cases even for such heavy quarks.
$π$-$N$ $σ$ term and proton axial vector matrix elements are calculated including disconnected contributions with a variant wall source method using the Wilson quark action at $β=5.7$ in quenched QCD. For the $σ$ term, we find $σ_{disc}/σ_{conn}=2.35(46)$ and $σ=44(6)$MeV--60(9)MeV. The fraction of proton spin carried by quarks is $ΔΣ=Δ{u}+Δ{d}+Δ{s}=+0.638(54)-0.347(46)-0.109(30)= +0.18(10)$.
Charmonium spectroscopy with Kogut-Susskind valence quarks are carried out for quenched QCD at $β=6.0$ and for two-flavor full QCD at $β=5.7$. Results for 1P--1S mass splitting and estimates of $α^{(5)}_{\overline{MS}}(m_Z)$ are reported. Problems associated with flavor breaking effects and finite size effects of $1P$ states are discussed.
We calculate both connected and disconnected contribution to the $π$-$N$ $σ$-term in quenched lattice QCD with Wilson quark action on a $12^3\times 20$ lattice at $β=5.7$. The latter is evaluated with the aid of the variant wall source method, which was previously applied successfully for extraction of $π$-$π$ scattering lengths and $η^\prime$ meson mass. We found that the disconnected contribution is about twice larger than the connected one. The value for the full $π$-$N$ $σ$ term $σ=40-60$ MeV is consistent with the experimental estimates. The nucleon matrix element of the strange quark density $\bar s s$ is fairly large in our result.
We demonstrate that sea quark effects of a magnitude expected from renormalization group considerations are clearly visible in the strong coupling constant measured in current full QCD simulations. Building on this result an estimate of $α_{\overline{MS}}^{(5)}(M_Z)$ is made employing the charmonium $1S-1P$ mass splitting calculated on full QCD configurations generated with two flavors of dynamical Kogut-Susskind quarks to fix the scale.
An exploratory study is made of the nucleon-nucleon $s$-wave scattering lengths in quenched lattice QCD with the Wilson quark action. The $π$-$N$ and $π$-$π$ scattering lengths are also calculated for comparison. The calculations are made with heavy quarks corresponding to $m_π/m_ρ\approx 0.73-0.95$. The results show that the $N$-$N$ system has an attractive force in both spin-singlet and triplet channels, with their scattering lengths significantly larger than those for the $π$-$N$ and $π$-$π$ cases, a trend which is qualitatively consistent with the experiment. Problems toward a more realistic calculation for light quarks are discussed.
Method of calculating hadron multi-point functions and disconnected quark loop contributions which are not readily accessible through conventional techniques is proposed. Results are reported for pion-pion, pion-nucleon and nucleon-nucleon scattering lengths and the flavor singlet-non singlet meson mass splitting estimated in quenched QCD.
We present numerical results and their analyses of finite-size effects of hadron masses for both quenched and full QCD calculations. We show that they are much larger for full QCD due to dynamical sea quarks and the associated breaking of $Z(3)$ symmetry. We also argue that finite-size effects are non-negligible even for the largest lattice size simulation currently being made for a very small quark mass. (talk at lattice93)
We present results showing that the strong coupling constant measured in two-flavor full QCD with dynamical Kogut-Susskind quarks at $β=5.7$ exhibit a 15\% increase due to sea quarks over that for quenched QCD at the scale $μ\approx 7$GeV . (talk at lattice93)
We investigate reheating of the universe by early formation of stars and quasars in the hierarchical clustering scheme of cold dark matter scenario, with perturbation fluctuations normalized by the COBE data. It is found that ionizing uv flux from OB stars with the abundance given by the standard initial mass function is strong enough to ionize the universe from $z\approx 30$ to the present epoch, if 1--2\% of the collapsed baryons go into stars. This lessens significantly the CMB anisotropies at a small angular scale. Reionization also increases the Jeans mass to $M_{\rm luminous}\approx 10^9M_\odot$ for $z\lsim 10$, which leads to a cut-off of the luminosity function of normal galaxies on a faint side. A strong uv flux is expected at $z\approx 2-5$, and the null result of the Gunn-Peterson test is naturally explained. Early star formation also results in production of heavy elements, and the observational metal abundance sets a strong constraint on the photon energy injection into the intergalactic space.
Recent observations suggest appreciable star formation activity in early-type galaxies down to redshift $z\sim 0.5$. If so, there is likely to be dust in these galaxies. We consider the possibility that obscuration by dust can reconcile the observed frequency of gravitational lensing of quasar images with the considerably larger rate predicted in a low density cosmologically flat universe dominated by a cosmological constant.