Resistance to extinction as a function of nonresponse incentive shift.
Resistance to extinction as function of nonresponse incentive shift in rats
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Light extinction photometer for measurement of particle sizes in polydispersions.
Particle size distribution determination by measuring light beam extinction in turbid medium with photometer
Adams, J. M.↗
Extinction in the far ultraviolet.
Interstellar grain model consisting of elongated dielectric particles represented by infinite circular cylinders reproducing observed interstellar extinction in IF far UV spectra
Greenberg, J. M.↗
Extinction by interstellar grains, Mie particles and polycyclic aromatic molecules.
Interstellar extinction models of classical Mie particles and quantum mechanical polycyclic aromatic molecules
Donn, B.↗
On the far-ultraviolet interstellar extinction law in the Orion nebula region.
Rocket measurement of far UV spectral intensity of theta Orionis for far UV interstellar extinction law in Orion nebula region
Carruthers, G. R.↗
Interstellar extinction in the ultraviolet. II.
Interstellar extinction in UV from zeta and epsilon Persei spectra obtained with scanner attached to telescope mounted in pointed Aerobee rocket
Stecher, T. P.↗
Measurements of the extinction parameters of hot seeded hydrogen at 1 atmosphere pressure
Extinction parameters of hydrogen aerosols at high temperatures
Clement, J. D.↗
Observations of atmospheric extinction from 0.315 to 1.06 microns
Atmospheric extinction observed photometrically in South Africa and southern France in narrow bands and astronomical UBV bands
Irvine, W. M.↗
Impure graphite grains and the interstellar extinction curve
Grains impurities effect on interstellar extinction curve from graphite grain model, discussing dirty ice coatings
Krishna, K. S.↗
A comparison between theoretical and experimental extinction behavior of composite solid propellants
Extinction model of composite solid propellant combustion including wall and flame heat release zones
Marxman, G. A.↗
Ultraviolet interstellar extinction from a comparison of epsilon Persei and zeta Persei
UV interstellar extinction from comparison of epsilon and zeta Persei, noting graphite features
Stecher, T. P.↗
Measurements of the extinction parameters of hot seeded hydrogen at high pressures
Measurement of extinction parameter of tungsten-hydrogen aerosols as function of wavelength at high pressures and temperatures
Clement, J. D.↗
The wavelength dependence of atmospheric extinction
Atmospheric extinction coefficients dependence on wavelength, comparing theoretical prediction to observational data
Blitzstein, W.↗
Supernovae and the extinction of the dinosaurs
Supernova explosion or solar outburst theory of climatic effects on mass extinction of organisms at Cretaceous-Tertiary boundary
Russell, D.↗
Structure in the interstellar-extinction curve
Fine structure of reddening interstellar extinction curves of stellar radiation, using photographic spectrophotometry
York, D. G.↗
Stellar ultraviolet colors and interstellar extinction
A sample of celescope results is studied. Most of the sample stars belong to the Orion and Vela regions. Stars with visual excess E(B-V) less than 0.05 are selected in order to derive relationships of intrinsic color index versus spectral type. The resulting intrinsic color-color relations are compared with existing blanketed and unblanketed model calculations. Finally, the preceding intrinsic relations are utilized to derive some results on interstellar extinction. Owing to the rather large scatter in the celescope data, the Vela stars give the more significant results because their visible excess E(B-V) is, in general, larger than that for the Orion stars.
Peytremann, E.↗
Fission xenon from extinct Pu-244 in 14,301.
Xenon extracted in step-wise heating of lunar breccia 14,301 contains a fission-like component in excess of that attributable to uranium decay during the age of the solar system. There seems to be no adequate source for this component other than Pu-244. Verification that this component is in fact due to the spontaneous fission of extinct Pu-244 comes from the derived spectrum which is similar to that observed from artificially produced Pu-244. It thus appears that Pu-244 was extant at the time lunar crustal material cooled sufficiently to arrest the thermal diffusion of xenon. Subsequent history has apparently maintained the isotopic integrity of plutonium fission xenon. Of major importance are details of the storage itself. Either the fission component is the result of in situ fission of Pu-244 and subsequent storage in 14,301 material, or the fission xenon was stored in an intermediate reservoir before incorporation into 14,301.
Drozd, R.↗