Thermal shock and erosion resistant tantalum carbide ceramic material

Ceramic tantalum carbide artifacts with high thermal shock and mechanical erosion resistance are provided by incorporating tungsten-rhenium and carbon particles in a tantalum carbide matrix. The mix is sintered by hot pressing to form the ceramic article which has a high fracture strength relative to its elastic modulus and thus has an improved thermal shock and mechanical erosion resistance. The tantalum carbide is preferable less than minus 100 mesh, the carbon particles are preferable less than minus 100 mesh, and the tungsten-rhenium particles are preferable elongate, having a length to thickness ratio of at least 2/1. Tungsten-rhenium wire pieces are suitable as well as graphite particles

Determination of elevated-temperature fatigue data on refractory alloys in ultra-high vacuum Fifth quarterly report, 1 Jul. - 1 Oct. 1965

Elevated-temperature fatigue data on notched and smooth specimens of refractory alloys in ultrahigh vacuum environment

Determination of elevated-temperature fatigue data on refractory alloys in ultra- high vacuum fourth quarterly report, 1 apr. - 1 jul. 1965

High temperature fatigue data on refractory alloys in ultrahigh vacuum - tests on titanium- zirconium-molybdenu

Combined high vacuum/high frequency fatigue tester

Apparatus permits application of significantly greater number of cycles or equivalent number of cycles in shorter time than conventional fatigue test machines. Environment eliminates problems associated with high temperature oxidation and with sensitivity of refractory alloy behavior to atmospheric contamination

Determination of elevated-temperature fatigue data on refractory alloys in ultra- high vacuum third quarterly report, 1 jan. - 1 apr. 1965

Fatigue data for refractory alloys at elevated temperatures in ultrahigh-vacuum environment

Magnetometer programming for DPS 2000 (system test set)

This ATM is a statement of the magnetometer processing currently included in the DPS 2000 computer programs being written for the ALSEP System Test Set.[prepared by R. Honeycutt, prepared by C. W. Coleman]

Observations of V592 Cas -— an Outflow at Optical Wavelengths

We present new red optical spectra of V592 Cas aimed at exploring the properties of the outflow of this system in a spectral region where the underlying white dwarf and the accretion disk do not contribute significantly to the observed absorption components of the Hα and He I line profiles. We use the Hα emission line to study the wind, which appears as pronounced blueshifted P Cygni absorption troughs whose low velocity end contaminates the blue side of the emission line profile. The wind appears to be episodic in nature, with multiple events reaching velocities of 5000 km s^–1 in Hα. Similar (but weaker) wind signatures appear in the He I 5876 Å line but are absent in He I 6678 Å. Our data suggest that during wind episodes the wind is phase dependent and is visible for half of the orbit of the system. Considering that V592 Cas is viewed almost face-on, the symmetry axis of the outflow cannot be orthogonal to the disk and/or the outflow must have some other inherent asymmetry in outflow geometry. A possible origin of the wind is in a disk hotspot, either at the initial impact point of the accretion stream on the disk edge or as a result of disk overflow (similar to SW Sextantis stars). Simultaneous optical photometry during one night of our spectroscopic observations indicate that there is no clear relationship between the optical brightness variations and the strength of the outflow in this system

Elevated temperature fatigue of TZC MOLYBDENUM alloy under high frequency and high vacuum conditions

Elevated temperature fatigue of TZC molybdenum alloy determined in high frequency and high vacuum test

Evidence for an accretion steam in the low-accretion-rate polar J2048

We present new red/near-infrared spectra of the low-accretion-rate polar J204827.9+005008.9. Compared to 2004 spectra in the literature, our 2008 data show more structured emission-line profiles. All emission lines in our spectra have two components at most orbital phases. The stronger component has a sinusoidal velocity variation (K~ 120 km s^(−1)) and is likely due to irradiation of the inner hemisphere of the secondary star by the white dwarf. Based on the appearance of the Hα Doppler tomogram, the weaker, larger amplitude, line component likely originates in a ballistic stream from the L1 point. J2048 is thought to be accreting via a wind from the secondary star, so the detection of velocity features consistent with the velocities of Roche lobe overflow is unexpected. It appears that J2048 was experiencing an interval of enhanced mass transfer during our observations. We briefly discuss scenarios that might lead to such a situation, such as changes in the chromospheric activity level on the secondary star