Particle theory

Abstract:

A critical review is given of the current status of cosmological nucleosynthesis. In the framework of the standard model with 3 types of relativistic neutrinos, the baryon-to-photon ratio, \eta, corresponding to the inferred primordial abundances of helium-4 and lithium-7 is presently ~2 \sigma below the value implied by the abundance of deuterium. The latter value is also coincident with the independent determination of \eta from WMAP observations of CMB anisotropy. However taking systematic uncertainties in the abundance estimates into account, there is overall concordance in the range \eta = (3.4 - 6.9) x 10^{-10} @ 95% c.l. corresponding to a cosmological baryon density \Omega_B h^2 = 0.012 - 0.025. If the above discrepancy is due to a neutrino chemical potential, then upto 7.1 effective neutrino species are allowed by nucleosynthesis. Other constraints on new physics are briefly discussed.

Abstract:

We test a variety of blocking and smearing algorithms for constructing glueball and string wave-functionals, and find some with much improved overlaps onto the lightest states. We use these algorithms to obtain improved results on the tensions of k-strings in SU(4), SU(6), and SU(8) gauge theories. We emphasise the major systematic errors that still need to be controlled in calculations of heavier k-strings, and perform calculations in SU(4) on an anisotropic lattice in a bid to minimise one of these. All these results point to the k-string tensions lying part-way between the 'MQCD' and 'Casimir Scaling' conjectures, with the power in 1/N of the leading correction lying ∈ [1,2]. We also obtain some evidence for the presence of quasi-stable strings in calculations that do not use sources, and observe some near-degeneracies between (excited) strings in different representations. We also calculate the lightest glueball masses for N = 2,..., 8, and extrapolate to N = ∞, obtaining results compatible with earlier work. We show that the N = ∞ factorisation of the euclidean correlators that are used in such mass calculations does not make the masses any less calculable at large N. © SISSA/ISAS 2004.