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Ballintine, J. E.

Publications and source records attributed to Ballintine, J. E..

6 records
All sourcesNASA NTRSDOE OSTI
NASA NTRS1984

Effective mobility limit in small-bubble, low-damping bubble materials

Examination of the implications of the basic equations that govern the motion of bubbles with nonzero winding number (S) yields an unexpected result. Bubble velocity is limited to the speed implied by the effective wall mobility (gamma)r/2S, no matter how large the actual wall mobility. For large bubbles, this limit will not usually be significant. However, for small bubbles (r less than 1 micron) in low-damping materials, this limit will profoundly affect the bubble motion. A derivation of the effect and experimental confirmation of it are presented.

Slusky, S. E. G.↗
NASA NTRS1977

Transient structure in the high-energy X-ray light curve of NP 0532

The paper reports the observation of pulsed fractions in the primary and secondary peaks, as well as in the interpulse region, of the high-energy X-ray light curve of NP 0532. A statistical analysis of light-curve data is performed, and a similar analysis is carried out using simulated data. It is concluded that a previously reported third peak in the light curve was transient in nature.

Ryckman, S. G.↗
NASA NTRS1976

The Perseus and Coma clusters of galaxies at energies above 20 keV

Observations of the Perseus and Coma clusters of galaxies were made on June 21, 1974, with a balloon-borne X-ray telescope (energies of approximately 20-150 keV). No positive detection was made. The data favor a thermal bremsstrahlung mechanism for the X-ray production in the Perseus cluster of galaxies over the inverse Compton mechanism. In the case of the Coma cluster of galaxies, the data are inconclusive with respect to determining the origin of the X-rays.

Scheepmaker, A.↗
NASA NTRS1976

Observations of Cygnus X-3 from a balloon-borne X-ray telescope

X-ray measurements in the energy range 20-150 keV were made from a balloon-borne telescope on June 1 1975. Three scans, centered at phases 0.45, 0.60, and 0.70, respectively, of the 4.8 hr cycle, were conducted. The observed relative intensity as a function of phase differs significantly from previously reported X-ray measurements.

Ricker, G. R.↗