On the linear stability of K\"ahler-Ricci solitons

This is a short note proving that K\"ahler-Ricci solitons with $\dim H^{(1,1)}(M)\ge 2$ are linearly unstable. This extends the results of Cao-Hamilton-Ilmanen in the K\"ahler-Einstein case.Comment: 11 pages; typos corrected, presentation improved and references added in v.

Convergence and Australian content: The importance of access

In the light of new and complex challenges to media policy and regulation, the Austrlaian government commissioned the Convergence Review in late 2010 to assess the continuing applicability and utility of the principles and objectives that have shaped the policy framework to this point. It proposed a range of options for policy change and identified three enduring priorities for continued media regulation: media ownership and control; content standards; and Australian content production and distribution. The purpose of this article is to highlight an area where we feel there are opportunities for further discussion and research: the question of how the accessibility and visibility of Australian and local content may be assured in the future media policy framework via a combination of regulation and incentives to encourage innovation in content distribution

A formalism for the construction of binary neutron stars with arbitrary circulation

Most numerical models of binary stars - in particular neutron stars in compact binaries - assume the companions to be either corotational or irrotational. Either one of these assumptions leads to a significant simplification in the hydrodynamic equations of stationary equilibrium. In this paper we develop a new formalism for the construction of binary stars with circulation intermediate between corotational and irrotational. Generalizing the equations for irrotational flow we cast the Euler equation, which is an algebraic equation in the case of corotational or irrotational fluid flow, as an elliptic equation for a new auxiliary quantity. We also suggest a parameterized decomposition of the fluid flow that allows for a variation of the stellar circulation.Comment: 8 pages, no figures; published version with erratu