The Einstein Redshift in White Dwarfs

Low-dispersion radial velocities of 53 white dwarfs have been measured on Palomar spectrograms. Table 1 contains the type, velocity, space-motion components, photometrically deduced temperature and radius, for each star. Table 4 contains 39 additional radial velocities of very low weight. A few members of wide binary systems and 6 white dwarfs in the Hyades provide direct measures of the Einstein gravitational redshift, with a mean value of +51 km/sec. Omitting the very-high-velocity star LP9-231, there are 37 DA stars, with a mean K-term (expansion velocity) of +65.6 km/sec. If the Hyades stars are omitted, the mean K term is +62.5 km/sec. A number of white dwarfs are members of the high-velocity population. Systematic wavelength shifts of He i lines in DB stars make their velocities more negative than those of DA stars; similar negative shifts may exist for metallic lines. The temperature scale is obtained from colors and, combined with luminosities, gives radii. The broad distribution of radii and redshifts is shown in Figure 2, and median values are derived. The median radial velocity for 37 DA stars is +58 km/sec, and the median radius 0.0107 R_⊙; the redshift and radius give a mass of 0.98 M_⊙. However, this value is almost certainly too high, if we expect accordance with the theoretical mass-radius relation. The theoretical M-R relation of a zero-temperature degenerate star predicts a redshift, for given mass, for various compositions. Two corrections could bring the theoretically expected redshifts into agreement with the observations. Either a systematic change in luminosity, ΔM_v of +0.25 mag, or a reciprocal temperature change of Δθ = —0.03, reduces the median radius to 0.0093 R_⊙. The mass derived from the redshift is then 0.86 M_⊙. These values are in accordance with the Hamada-Salpeter mass-radius relation, if the composition in the interior is pure helium. A carbon or magnesium interior also gives a radius not too different from the colorimetric radius. An iron core gives a mass of 0.73 M_⊙, but a radius of 0.008 R_⊙, sufficiently smaller to require substantial changes in the temperature scale. The mass now derived from the radial velocities is higher than that previously found from radii only and closer to the Chandrasekhar limit

Characterization of Piedmont Residual Soil and Saprolite in Maryland

Residual soils in the Eastern Piedmont Physiographic province are difficult to characterize because of the unique mineralogy and development of the soils. They are derived in place by weathering of the underlying gneiss and schist bedrock, and are characterized by a gradual transition from soil to decomposed-rock to rock with no clear demarcation between the strata. The soils generally consist of low plasticity micaceous clayey silts, sandy silts and silty sands. It is often difficult to obtain undisturbed samples of these soils and Intermediate Geo-Materials, so most shear strength and compressibility properties are derived from experience or correlations with index parameters such as the SPT N-value and Atterberg limits. For the State of Maryland’s Intercounty Connector (ICC) Project, the General Engineering Consultant (GEC), Intercounty Connector Corridor Partners (ICCCP) Joint Venture working directly for the Maryland State Highway Administration (MSHA), performed a Preliminary Geotechnical Subsurface Exploration (PGSE) during the procurement phase so that the Design-Build (DB) teams would develop preliminary designs on which to base their technical and price proposals. As part of the PGSE performed by the GEC for Contract A of the ICC, several undisturbed samples were obtained so that the shear strength parameters could be determined on relatively undisturbed samples. An attempt was made to correlate the SPT N-values and laboratory testing with seismic refraction geophysical exploration to estimate engineering parameters for design of cut slopes, shrink/swell, a cut/cover tunnel, and several bridges for the three general strata. Not only were undisturbed samples tested to determine the shear strength parameters, remolded samples, compacted to 95% of the modified Proctor maximum dry density, were also tested to determine the remolded shear strength parameters for embankment construction

Preliminary report on IUE spectra of the Crab Nebula

The Crab Nebula is marginally observable with the IUE. Observations of the optically brightest filamentary regions, made with IUE in August 1979, show the C IV lambda 1549, He II lambda 1640, and C III lambda 1909 emission lines. The intensities of these lines were compared with the visual wavelength data. It appears that carbon is not overabundant in the Crab; carbon/oxygen is approximately normal and oxygen is slightly scarcer than normal as a fraction of the total mass

Tied-Back Top-Down Wall to Support I-295 Ramp

Woodrow Wilson Replacement Bridge Project included widening the Washington Beltway (I-95/I-495) Outer Loop from three lanes to six-lanes. This required supporting two existing ramps that connect I-295 and MD 210 as well as the existing Mechanically Stabilized Earth (MSE) wall that supports the ramps. The MSE is about 17-ft tall, about 570-ft long, and at the top of a slope. A tied-back soldier pile and lagging wall with cast-in-place facing was selected to support the MSE and the ramps. The new wall will be about 1,376-ft long and will be as high as 37-ft. The closest approach of the wall to the existing MSE is about 3-ft. Laboratory testing was supplemented with Dilatometer Test (DMT) and Cone Penetration Test (CPT) soundings. PYWall and PLAXIS were used to estimate wall deflections and bending moments in the soldier piles. This paper reviews the analysis techniques, describes the design and the construction methods, and the instrumentation used to monitor the wall and MSE movements. The results of the computer simulations were compared to the inclinometer results. As work progressed simulations were updated by modifying the soil parameters to obtain calculated results that are more nearly consistent with the instrumentation readings

Possible Observational Criteria for Distinguishing Brown Dwarfs from Planets

The difference in formation process between binary stars and planetary systems is reflected in their composition as well as their orbital architecture, particularly orbital eccentricity as a function of orbital period. It is suggested here that this difference can be used as an observational criterion to distinguish between brown dwarfs and planets. Application of the orbital criterion suggests that with three possible exceptions, all of the recently-discovered substellar companions discovered to date may be brown dwarfs and not planets. These criterion may be used as a guide for interpretation of the nature of sub-stellar mass companions to stars in the future.Comment: LaTeX, 11 pages including 2 figures, accepted for publication in the Astrophysical Journal Letter

Nurses\u27 Alumnae Association Bulletin - Volume 2 Number 2

Coming Events Come On, \u2732 Ballot for Officers Hospital News Legislation Scholarship Fund Notes Refresher Course Correspondence Use of Heparin in Modern Treatment The Jefferson Medical College Library Nursing School Education Action - Camera - Seniors Degrees Received Engagements Weddings Births Deaths Attention Alumnae Bulletin Progress Of Special Interest Army Assignments Organized Staff Meeting

Implementation of lean manufacturing techniques for the replenishment of purchased parts used at a tier one automobile supplier

Thesis (S.M.)--Massachusetts Institute of Technology, Sloan School of Management; and, (S.M.)--Massachusetts Institute of Technology, Dept. of Mechanical Engineering, 1999.Includes bibliographical references (leaf 163).by Derek L. Trimble.S.M

The Einstein Redshift in White Dwarfs

Low-dispersion radial velocities of 53 white dwarfs have been measured on Palomar spectrograms. Table 1 contains the type, velocity, space-motion components, photometrically deduced temperature and radius, for each star. Table 4 contains 39 additional radial velocities of very low weight. A few members of wide binary systems and 6 white dwarfs in the Hyades provide direct measures of the Einstein gravitational redshift, with a mean value of +51 km/sec. Omitting the very-high-velocity star LP9-231, there are 37 DA stars, with a mean K-term (expansion velocity) of +65.6 km/sec. If the Hyades stars are omitted, the mean K term is +62.5 km/sec. A number of white dwarfs are members of the high-velocity population. Systematic wavelength shifts of He i lines in DB stars make their velocities more negative than those of DA stars; similar negative shifts may exist for metallic lines. The temperature scale is obtained from colors and, combined with luminosities, gives radii. The broad distribution of radii and redshifts is shown in Figure 2, and median values are derived. The median radial velocity for 37 DA stars is +58 km/sec, and the median radius 0.0107 R_⊙; the redshift and radius give a mass of 0.98 M_⊙. However, this value is almost certainly too high, if we expect accordance with the theoretical mass-radius relation. The theoretical M-R relation of a zero-temperature degenerate star predicts a redshift, for given mass, for various compositions. Two corrections could bring the theoretically expected redshifts into agreement with the observations. Either a systematic change in luminosity, ΔM_v of +0.25 mag, or a reciprocal temperature change of Δθ = —0.03, reduces the median radius to 0.0093 R_⊙. The mass derived from the redshift is then 0.86 M_⊙. These values are in accordance with the Hamada-Salpeter mass-radius relation, if the composition in the interior is pure helium. A carbon or magnesium interior also gives a radius not too different from the colorimetric radius. An iron core gives a mass of 0.73 M_⊙, but a radius of 0.008 R_⊙, sufficiently smaller to require substantial changes in the temperature scale. The mass now derived from the radial velocities is higher than that previously found from radii only and closer to the Chandrasekhar limit

All-solid-state electrochromic reflectance device for emittance modulation in the far-infrared spectral region

All-solid-state electrochromic reflectance devices for thermal emittance modulation were designed for operation in the spectral region from mid- to far-infrared wavelengths (2–40 μm). All device constituent layers were grown by magnetron sputtering. The electrochromic (polycrystalline WO3), ion conductor (Ta2O5), and Li+ ion-storage layer (amorphous WO3), optimized for their infrared (IR) optical thicknesses, are sandwiched between a highly IR reflecting Al mirror, and a 90% IR transmissive Al grid top electrode, thereby meeting the requirements for a reversible Li+ ion insertion electrochromic device to operate within the 300 K blackbody emission range. Multicycle optical switching and emittance modulation is demonstrated. The measured change in emissivity of the device is to 20%

Farm and Ranch Credit.

12 p