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California at San Diego, La Jolla, California 92093 (Received 29 September 1989) The free energy of the classical ,,;,= 178--180. This paper presents an analytic calculation of the free energy of the solid phase for both bcc and face-centered-cubic (fcc) lattices. The 0( T ) term in the free energy gives the lowest

or semiconductor. Pattern is chosen so that strain (to be measured) . . . . . . occurs along direction of current the gauge factor. For metal strain gauges, Gf = 2. (An integer!) For semiconductor strain gauges Gf is much resistance R0(T) is a function of temperature. Conditioning circuit must "remove" R0(T) term. A bridge does

for cogeneration - either topp ng or bottoming systems - which are fuel flexible. Achievements to date include sho tterm operation of a diesel using a coal-wat r slurry as a fuel; testing of an improved vaporizer for organic Rankine cycle bottomi g systems... rugged and less susceptible to joint leakage prob lems, corrosion, fouling and breakage. The waste heat recovery program includes work in advanced heat pumps utilizing chemical absorp tion systems, chemical heat of reaction sys tems and magnetic...

. Khovanskii?s results imply that a square system of n real polynomial equations in n variables with total tterms has at most (n+1)t2t(t?1)/2 non-degenerate roots in the positive orthant. Khovanskii?s bound was improved by the work of F. Bihan and F. Sottile.... For more details see [12], [15], [17] and [21]. 1. What Are the p-adic Numbers? Let Q denote the set of rational numbers, we can construct a norm on Q in the following way: Let p be a prime number, and for any integer a ? Z, define the p-adic valuation of a...

We propose a large class of nonsingular cosmologies of arbitrary spatial curvature whose cosmic history is determined by a primeval dynamical $\\Lambda (t)$-term. For all values of the curvature, the models evolve between two extreme de Sitter phases driven by the relic time-varying vacuum energy density. The transition from inflation to the radiation phase is universal and points to a natural solution of the graceful exit problem regardless of the values of the curvature parameter. The flat case recovers the scenario recently discussed in the literature (Perico et al., Phys. Rev. D88, 063531, 2013). The early de Sitter phase is characterized by an arbitrary energy scale $H_I$ associated to the primeval vacuum energy density. If $H_I$ is fixed to be nearly the Planck scale, the ratio between the relic and the present observed vacuum energy density is $\\rho_{vI}/\\rho_{v0} \\simeq 10^{123}$.

Lorentz violation is a candidate quantum-gravity signal, and the Standard-Model Extension (SME) is a widely used parametrization of such violation. In the gravitational SME sector, there is an elusive coefficient for which no effects have been found. This is is known as the $t$ puzzle and, to date, it has no compelling explanation. In this paper, several approaches to understand the $t$ puzzle are proposed. First, redefinitions of the dynamical fields are studied, which reveal that other SME coefficients can be moved to nongravitational sectors. It is also shown that the gravity SME sector can be treated \\textit{\\`a la} Palatini, and that, in the presence of spacetime boundaries, it is possible to correct its action to get the desired equations of motion. Also, through a reformulation as a Lanczos-type tensor, some problematic features of the $t$ term, that should arise at the phenomenological level, are revealed. Additional potential explanations to the $t$ puzzle are outlined.

Lorentz violation is a candidate quantum-gravity signal, and the Standard-Model Extension (SME) is a widely used parametrization of such violation. In the gravitational SME sector, there is an elusive coefficient for which no effects have been found. This is is known as the $t$ puzzle and, to date, it has no compelling explanation. In this paper, several approaches to understand the $t$ puzzle are proposed. First, redefinitions of the dynamical fields are studied, which reveal that other SME coefficients can be moved to nongravitational sectors. It is also shown that the gravity SME sector can be treated \\textit{\\`a la} Palatini, and that, in the presence of spacetime boundaries, it is possible to correct its action to get the desired equations of motion. Also, through a reformulation as a Lanczos-type tensor, some problematic features of the $t$ term, that should arise at the phenomenological level, are revealed. Additional potential explanations to the $t$ puzzle are outlined.