N ov 2 01 4 A renormalisation group method . IV . Stability analysis

5 N ov 2 01 4 A renormalisation group method . II . Approximation by local polynomials

This paper is the second in a series devoted to the development of a rigorous renormalisation group method for lattice field theories involving boson fields, fermion fields, or both. The method is set within a normed algebra N of functionals of the fields. In this paper, we develop a general method—localisation—to approximate an element of N by a local polynomial in the fields. From the point o...

ar X iv : 1 01 1 . 54 92 v 1 [ nl in . C D ] 2 4 N ov 2 01 0 Chimera states in coupled sine - circle map lattices

Systems of coupled oscillators have been seen to exhibit chimera states, i.e. states where the system splits into two groups where one group is phase locked and the other is phase randomized. In this work, we report the existence of chimera states in a system of two interacting populations of sine circle maps. This system also exhibits the clustered chimera behavior seen earlier in delay couple...

ar X iv : h ep - p h / 01 11 17 2 v 1 1 4 N ov 2 00 1 Summary of Working Group 1 : Theory Part

I will summarize theoretical issues in Working Group 1 at Nufact’01. In particular I will clarify a controversy on the optimum baseline L muon energy Eμ for measurements of the CP phase at a neutrino factory. If the uncertainty of the matter effect is assumed to be ±10%, which may be slightly too pessimistic, then the results from two groups agree (L ∼ 1000km, Eμ ∼ 10GeV).

ar X iv : m at h - ph / 0 31 10 01 v 4 3 N ov 2 00 4 Clifford Valued Differential Forms , Algebraic Spinor Fields

ar X iv : 1 10 1 . 54 01 v 2 [ gr - q c ] 1 5 Ju n 20 11 Asymptotically Safe Cosmology

We study quantum modifications to cosmology in a Friedmann-Robertson-Walker universe with and without scalar fields by taking the renormalisation group running of gravitational and matter couplings into account. We exploit the Bianchi identity to relate the renormalisation group scale with scale factor and derive the improved cosmological evolution equations. We find two types of cosmological f...