An examination of strategic opportunities provided by the conference committee procedure in the U.S. Congress

Deference to committees in Congress has been a much studied phenomena for close to 100 years. This deference can be characterized as the unwillingness of a potentially winning coalition on the House floor to impose its will on a small minority, a standing committee. The congressional scholar is then faced with two problems: observing such deference to committees, and explaining it. Shepsle and Weingast have proposed the existence of an ex-post veto for standing committees as an explanation of committee deference. They claim that as conference reports in the House and Senate are considered under a rule that does not allow amendments, the conferees enjoy agenda-setting power. In this paper I describe a test of such a hypothesis (along with competing hypotheses regarding the effects of the conference procedure). A random-utility model is utilized to estimate legislators' ideal points on appropriations bills from 1973 through 1980. I prove two things: 1) that committee deference can not be said to be a result of the conference procedure; and moreover 2) that committee deference does not appear to exist at all.

Origin of Th/U variations in chondritic meteorites

Isotope dilution thorium and uranium analyses of the Harleton chondrite show a larger scatter than previously observed in equilibrated ordinary chondrites (EOC). The linear correlation of Th/U with 1/U in Harleton (and all EOC data) is produced by variation in the chlorapatite to merrillite mixing ratio. Apatite variations control the U concentrations. Phosphorus variations are compensated by inverse variations in U to preserve the Th/U vs. 1/U correlation. Because the Th/U variations reflect phosphate ampling, a weighted Th/U average should converge to an improved solar system Th/U. We obtain Th/U=3.53 (1<sub>-meansub>=0.10), significantly lower and more precise than previous estimates.

To test whether apatite also produces Th/U variation in CI and CM chondrites, we performed P analyses on the solutions from leaching experiments of Orgueil and Murchison meteorites.

A linear Th/U vs. 1/U correlation in CI can be explained by redistribution of hexavalent U by aqueous fluids into carbonates and sulfates.

Unlike CI and EOC, whole rock Th/U variations in CMs are mostly due to Th variations. A Th/U vs. 1/U linear correlation suggested by previous data for CMs is not real. We distinguish 4 components responsible for the whole rock Th/U variations: (1) P and actinide-depleted matrix containing small amounts of U-rich carbonate/sulfate phases (similar to CIs); (2) CAIs and (3) chondrules are major reservoirs for actinides, (4) an easily leachable phase of high Th/U. likely carbonate produced by CAI alteration. Phosphates play a minor role as actinide and P carrier phases in CM chondrites.

Using our Th/U and minimum galactic ages from halo globular clusters, we calculate relative supernovae production rates for <sup>232sup>Th/<sup>238sup>U and <sup>235sup>U/<sup>238sup>U for different models of r-process nucleosynthesis. For uniform galactic production, the beginning of the r-process nucleosynthesis must be less than 13 Gyr. Exponentially decreasing production is also consistent with a 13 Gyr age, but very slow decay times are required (less than 35 Gyr), approaching the uniform production. The 15 Gyr Galaxy requires either a fast initial production growth (infall time constant less than 0.5 Gyr) followed by very low decrease (decay time constant greater than 100 Gyr), or the fastest possible decrease (≈8 Gyr) preceded by slow in fall (≈7.5 Gyr).

Representing measures on the Royden boundary for solutions of Δu=Pu on a Riemannian manifold

Consider the Royden compactification R* of a Riemannian n-manifold R, Γ = R*\R its Royden boundary, Δ its harmonic boundary and the elliptic differential equation Δu = Pu, P ≥ 0 on R. A regular Borel measure m<sup>Psup> can be constructed on Γ with support equal to the closure of Δ<sup>Psup> = {q ϵ Δ : q has a neighborhood U in R* with _U<sup>ʃsup><sub>ᴖRsub><sup>P ˂ ∞ sup>}. Every enegy-finite solution to u (i.e. E(u) = D(u) + <sup>ʃsup><sub>Rsub>u<sup>2sup>P ˂ ∞, where D(u) is the Dirichlet integral of u) can be represented by u(z) = <sup>ʃsup><sub>Γsub>u(q)K(z,q)dm<sup>Psup>(q) where K(z,q) is a continuous function on <sup>Rxsup> Γ . A <sub>Psub><sup>~sup><sub>Esub>-function is a nonnegative solution which is the infimum of a downward directed family of energy-finite solutions. A nonzero <sub>Psub><sup>~sup><sub>Esub>-function is called <sub>Psub><sup>~sup><sub>Esub>-minimal if it is a constant multiple of every nonzero <sub>Psub><sup>~sup><sub>Esub>-function dominated by it. <u>THEOREMu>. There exists a <sub>Psub><sup>~sup><sub>Esub>-minimal function if and only if there exists a point in q ϵ Γ such that m<sup>Psup>(q) > 0. <u>THEOREMu>. For q ϵ Δ<sup>Psup> , m<sup>Psup>(q) > 0 if and only if m<sup>0sup>(q) > 0 .