We study the critical behaviour of the chira! phase transition of SU(3) lattice QCD with one species of staggered fermions in the strong coupling limit. We find a second-order phase transition which seems to be controlled by an effective action which is in the same universality class as three-dimensional 0(2) spin models. In particular, we find for the exponent b, 0.18 < 1/~<0.25, in good agreement with the three-dimensional 0(2) value, 1/b 0.21.

Fourier transform ion cyclotron resonance mass spectrometry (FTICR-MS) is often limited by space-charge effects. Previously, particle-in-cell (PIC) simulations have been used to understand these effects on FTICR-MS signals. However, none have extended fully into the space-charge dominated (plasma) regime. We use a two-dimensional (2-D) electrostatic PIC code, which facilitates work at very high number densities at modest computational cost to study FTICR-MS in the plasma regime. In our simulation, we have observed peak coalescence and the rapid loss of signal coherence, two common experimental problems. This demonstrates that a 2-D model can simulate these effects. The 2-D code can handle a larger numbers of particles and finer spatial resolution than can currently be addressed by 3-D models. The PIC method naturally takes into account image charge and space charge effects in trapped-ion mass spectrometry. We found we can quantify the relative abundances of two closely spaced (such as 7 Be ϩ and 7 Li ϩ ) species in the plasma regime even when their peaks have coalesced. We find that the frequency of the coalesced peak shifts linearly according to the relative abundances of these species. Space charge also affects more widely spaced lines. Singlyionized 7 BeH and 7 Li have two separate peaks in the plasma regime. Both the frequency and peak area vary nonlinearly with their relative abundances. Under some conditions, the signal exhibited a rapid loss of coherence. We found that this is due to a high order diocotron instability growing in the ion cloud. (J

Presented herein are measurements of the solar wind electron number density and temperature near and within the bow shock of Venus. The measurements were made by the Pioneer Venus mission Orbiter Retarding Potential Analyzer operating in its suprathermal electron mode. The measurements are essentially point measurements. The spacecraft travels approximately 0.8 km during the 0.1 s time interval required to record a single I‐V curve. The dual measurement of a density and temperature is obtained from one sweep by least squares fitting a mathematical Maxwellian expression to the I‐V curve. The distance between successive measurements is approximately 100 km. In many orbits, when the spacecraft is crossing or traveling within the bow shock, the derived densities and temperatures (high density, high temperature (HDHT)) are large, densities of the order of 100 cm−3 and temperatures of the order of several hundred eV. We interpret these HDHT measurements as measurements in regions where the large, directed kinetic energy of the solar wind ions is being degraded into randomized, more thermal‐like energy distributions of the electrons and ions through wave‐particle interactions. The HDHT values define the electron energy distribution in the limited energy interval 0 to 50 eV. We assume that the underlying electron flux distributions are flat topped like those measured in the Earth's bow shock. We also report densities and temperatures of EUV produced photoelectron energy distributions measured within the ionosphere.

In an effort to make data on the reflectivity and transmission of multilayer optical elements more usable, we have developed a computer code for the manipulation and graphical display of a general data set consisting of x, y, and delta -y values. The code was developed for a DEC VAX computer running a version 4.2 or later VMS operating system. Facilities are available for algebraic manipulation, editing, smoothing, interpolating, and deconvolving data sets in a straightforward way. The code is entirely self -contained with the exception of the graphics output support, which is centralized to allow for simple interfacing to the graphics package resident on the target system. The capabilities of the code are described and sample output is shown.

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