The orbit of the Cepheid AW Per

An orbit for the classical Cepheid AW Per was derived. Phase residuals from the light curve are consistent with the light-time effect from the orbit. The companion was studied using IUE spectra. The flux distribution from 1300 to 1700 A is unusual, probably an extreme PbSi star, comparable to a B7V or B8V star. The flux of the composite spectrum from 1200 A through V is well matched by F7Ib and B8V standard stars with Delta M(sub upsilon) = 3(m) multiplied by 1. The mass function from the orbit indicates that the mass of the Cepheid must be greater that 4.7 solar mass if it is the more massive component. A B7V to B8V companion is compatible with the 1 sigma lower limit (3.5 solar mass) from the mass function. This implies that the Cepheid has the same mass, but the large magnitude difference rules this out. It is likely that the companion is itself a binary

Fundamental Parameters of Cepheids: Masses and Multiplicity

Masses determined from classical Cepheids in binary systems are a primary test of both pulsation and evolutionary calculations. The first step is to determine the orbit from ground-based radial velocities. Complementary satellite data from Hubble, FUSE, IUE, and Chandra provide full information about the system. A summary of recent results on masses is given. Cepheids have also provided copious information about the multiplicity of massive stars, as well as the distribution of mass ratios and separations. This provides some important constraints for star formation scenarios including differences between high and low mass results and differences between close and wide binaries

Fiscal equity of teacher salary and compensation in Oklahoma .

This quantitative study investigated the equitable distribution of resources to determine their accessibility to all children attending public schools in Oklahoma. With No Child Left Behind (NCLB) schools are mandated to employ "highly qualified" teachers. Teachers are an important resource and their significance is emphasized more as schools attempt to increase student achievement. Every student educated in Oklahoma should have an equal right to educational resources. Teacher salaries consume the largest portion of the educational budgets and an investigation of salaries and compensation as a resource was warranted. This study investigated two fiscal years; 2000, the year before a $3000 pay raise was awarded, and 2005, the most recent year after the pay raise. Descriptive statistics were used to determine horizontal equity and with correlations, regression analysis, the Gini coefficient, and McLoone index used to determine wealth neutrality. Instructional salaries and total instructional compensation were inequitably distributed in Oklahoma and the degree of inequity increased from fiscal years 2000 to 2005. Wealth neutrality was examined using both the Gini coefficient and McLoone index and it was determined that the distribution of resources was dependent upon where a student resides. Four variables, assessed property valuation, socioeconomic status, percentage of Caucasian students, and proximity to a bordering state were investigated to determine their impact on the distribution of resources. All variables, except the percentage of Caucasian students, were found to significantly influence the distribution of resources. This study exposed some inequities that exist in the distribution of instructional salaries and total instructional compensation in Oklahoma thus preventing all students who are educated in our public schools from receiving equal access to resources that determine the quality of educational instruction the student receives

Cepheid binaries with large mass ratios (M1/M2)

The IUE observations of 3 Cepheid systems (Polaris, FF Aql, and S Sge) are used to derive, or set limits on, the temperatures and masses of the companions. Light from the companions of FF Aql and S Sge from 1700 to 2000 A is consistent with an A5 to A7 main sequence companion for both Cepheids, with a mass of 1.8 solar mass. This mass for the companion of S Sge is smaller than required by the orbital mass function and an evolutionary mass of the Cepheid, suggesting that the companion may itself be a binary. For Polaris, the mass of the companion must be less than 1.8 solar mass