ASYMPTOTICALLY FREE FLUIDS
I study the field theory of a scalar field ..omega.. with solely cubic interactions in three dimensions: (..omega../sup 3/)/sub 3/. I insist that the ..omega.. field represents the density of a fluid, so ..omega.. must always be > or =0. If there are long-range couplings in the fluid such that the inverse ..omega.. propagator is linear rather than quadratic in momentum, then (..omega../sup 3/)/sub 3/ theory is asymptotically free. The asymptotic freedom of (..omega../sup 3/)/sub 3/ theory is closely related to the existence of a nonzero, ultraviolet-stable fixed point in large-N (phi-bar/sup 6/)/sub 3/ theory. There are also analogies between the asymptotic freedom of fluids (in three and six dimensions) and that of non-Abelian gauge fields (in four dimensions).

title: Damping rates for moving particles in hot QCD.
abstract: Using a program of perturbative resummation I compute the damping rates for fields at nonzero spatial momentum to leading order in weak coupling in hot QCD. Sum rules for spectral densities are used to simplify the calculations. For massless fields the damping rate has an apparent logarithmic divergence in the infrared limit, which is cut off by the screening of static magnetic fields ("magnetic mass"). This demonstrates how at high temperature even perturbative quantities are sensitive to nonperturbative phenomena.

title: Theory at quark matter '02
abstract: I summarize theory at Quark Matter '02, stressing the continuing inability model to describe all notable features of the data from √ s /A: 55 → 200GeV

title: Soft Amplitudes in Hot Gauge Theories: A General Analysis
abstract: A systematic method for the calculation of amplitudes in hot gauge theories is developed. It is necessary to distinguish between hard momenta (of order T ) and soft momenta (of order gT ). Ordinary perturbation theory applies at hard momenta, but over soft momenta, effective propagators and vertices are required. These effective quantities resum the leading contributions from thermal fluctuations with hard virtual momenta. These “hard thermal loops” arise solely from subdiagrams at one-loop order: they are ultraviolet finite, gauge independent, and satisfy simple Ward identities. To illustrate the method we apply it to the quark and gluon self-energies. Ward identities are used to show that to one-loop order in this effective perturbation expansion, the two-point T -matrix elements constructed from the self-energies are gauge invariant. This proves that to leading order in g , the quark and gluon damping rates are gauge invariant.

title: Cool pions move at less than the speed of light
abstract: At nonzero temperature, pions propagate through a thermal medium at less than the speed of light. About low temperature, this effect begins not at $\sim T^2$, but at next to leading order, $\sim T^4$. We also derive the generalization of the relation of Gell-Mann, Oakes, and Renner to nonzero temperature.

title: Nonabelian Debye screening, tsunami waves, and worldline fermions
abstract: I give a pedagogical review of the derivation for the effective lagrangian for nonabelian Debye screening, or hard thermal loops. Following Kelly, Liu, Lucchesi, and Manuel, I give the simplest derivation possible, using classical kinetic theory. 
The result is valid not just for a thermal, but for an arbitrary initial distributions. I use this to study the evolution, at short times, of a gluonic ``tsunami wave''. 
I also suggest how classical kinetic theory may arise at one loop order. Using the wordline representation of the one loop effective action, I follow D'Hoker and Gagn\'{e} to replace the Wilson line by an integral over worldline fermions. A bilinear of these worldline fermions naturally defines a nonabelian charge, whose equation of motion is Wong's equation.

title: The ROSAT HRI X-Ray Survey of the Cygnus Loop
abstract: We describe and report progress on the joint U.S. and German campaign to map the X-ray emission from the entire Cygnus Loop with the ROSAT High Resolution Imager. The Cygnus Loop is the prototype for a supernova remnant that is dominated by interactions with the interstellar medium and supplies fundamental physical information on this basic mechanism for shaping the interstellar medium. The global view that these high-resolution (FWHM ~ 10'') observations provide emphasizes the inhomogeneity of the interstellar medium and the pivotal nature of cloud-blast-wave interactions in determining the X-ray morphology of the supernova remnant. While investigating the details of the evolution of the blast wave, we also describe the interstellar medium in the vicinity of the Cygnus Loop, which the progenitor star has processed. Although we do not expect the X-ray observations to be complete until 1997 September, the incomplete data combined with deep Hα images provide definitive evidence that the Cygnus Loop was formed by an explosion within a preexisting cavity.