The Complete |Delta S|=2 Hamiltonian in the Next-To-Leading Order

We present the complete next-to-leading order short-distance QCD corrections to the effective \dstwo -hamiltonian in the Standard Model. The calculation of the coefficient $\eta_3$ is described in great detail. It involves the two-loop mixing of bilocal structures composed of two \dsone\ operators into \dstwo\ operators. The next-to-leading order corrections enhance $\eta_3$ by 27\% to \eta_3=0.47 \errorpm{+0.03}{-0.04} thereby affecting the phenomenology of $\epsilon_K$ sizeably. $\eta_3$ depends on the physical input parameters $m_t$, $m_c$ and \laMSb only weakly. The quoted error stems from renormalization scale dependences, which have reduced compared to the old leading log result. The known calculation of $\eta_1$ and $\eta_2$ is repeated in order to compare the structure of the three QCD coefficients. We further discuss some field theoretical aspects of the calculation such as the renormalization group equation for Green's functions with two operator insertions and the renormalization scheme dependence caused by the presence of evanescent operators.Comment: 68 pages, requires LaTeX2e and the standard LaTeX-packages epsf.sty, rotate.sty, a4.sty, subeqn.sty, cite.sty, array.sty, dcolumn.sty; Figures are submitted as a seperate tar.gz-file. A complete PostScript version may be obtained from ftp://feynman.t30.physik.tu-muenchen.de/pub/preprints/tum-86-96.ps.gz or ftp://feynman.t30.physik.tu-muenchen.de/pub/preprints/tum-86-96.ps2.gz (scaled down and rotated version to print two pages on one sheet of paper). Source available at ftp://feynman.t30.physik.tu-muenchen.de/pub/preprints/tum-86-96.tar.g

Cosmological implications of neutrinos

Massive neutrinos were the first proposed, and remain the most natural, particle candidate for the dark matter. In the absence of firm laboratory evidence for neutrino mass, considerations of the formation of large scale structure in the universe provide a sensitive, albeit indirect, probe of this possibility. Observations of galaxy clustering and large angle anisotropy in the cosmic microwave background have been interpreted as requiring that neutrinos provide about 20% of the critical density. However the need for such `hot' dark matter is removed if the primordial spectrum of density fluctuations is tilted below scale-invariance, as is often the case in physically realistic inflationary models. This question will be resolved by forthcoming precision measurements of microwave background anisotropy on small angular scales. This data will also improve the nucleosynthesis bound on the number of neutrino species and test whether decays of relic neutrinos could have ionized the intergalactic medium.Comment: 13 pages (LaTeX, espcrc2.sty) including 9 figures (epsf); Plenary talk at the XVI International Workshop on Weak Interactions and Neutrinos, Capri, 22-28 June 1997; to appear in the Proceedings (eds. G. Fiorillo, V. Palladino and P. Strolin) ; References [11,28,52] revise