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Search indexed NASA NTRS and DOE OSTI research on propulsion, heat transfer, battery materials and energy systems. Follow report and document links to the original sources.

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At least 91 records · Page 5
All sourcesNASA NTRSDOE OSTI
NASA NTRS1985

High-resolution spectroscopic observation of Vela X-1 in the hard X-ray energy range

The first high resolution (1.2 keV FWHM hard X-ray equal to or greater than 20 keV) observation of Vela X-1 is reported. Data were accumulated during a 5 hour balloon flight launched on December 5, 1984. A summed epoch analysis yields a light curve and period (283 sec) consistent with previous measurements. Significant pulsations were present to an energy of 60 keV. No statistically significant features were observed in the energy spectrum and the spectrum is well fit (x sup 2 = 17.8 for 16 d.o.f.) by a simple exponential spectrum with an E folding length of 10.8 + or - 1.0 keV.

Tueller, J.↗
DOE OSTI2022

Expanding the Energy Range from eV to MeV and Fabrication of Sources Enabling Novel Focused Ion Beam Nanofabrication and Modification

Multi-species focused ion beam (FIB) has the capability of running a variety of ion species allowing tailoring of the ion to the application enabling new applications of FIB such as localized doping and the creation of single defect centers. Also, through variation of the ion energy from eV to MeV, specific depths within the sample can be targeted enabling targeting of deeply buried layers inaccessible by traditional FIB systems. The combination of these capabilities opens up new areas of study including quantum information science and 2D materials.

47 OTHER INSTRUMENTATION↗
NASA NTRS1985

Primary cosmic ray spectrum in the 10 to the 12th power - 10 to the 16th power eV energy range from the NUSEX experiment

A primary cosmic ray spectrum was derived which fits both experimental multiple muon rates and the all-nucleon flux derived from the single muon intensities underground. In the frame of the interaction model developed by Gaisser, Elbert and Stanev, it is possible to reproduce NUSEX muon data with a primary composition in which the iron spectrum is only slightly flatter than the proton one. This result rules out the popular idea that the primary composition varies drastically with increasing energy, leading to the dominance of heavier nuclei at energies 10 to the 15th power to 10 to the 16th power eV.

Battistoni, G.↗
NASA NTRS1971

Observations of the scatter-free solar-flare electrons in the energy range 20-1000 keV

Observations of the scatter-free electron events from solar active region McMath No. 8905 are presented. The measurements were made on Explorer 33 satellite. The data show that more than 80% of the electrons from these events undergo no or little scattering and that these electrons travel only approximately 1.5 a.u. between the sun and the earth. The duration of these events cannot be accounted fully by velocity dispersion alone. It is suggested that these electrons could be continuously injected into interplanetary medium for a time interval of approximately 2 to 3 minutes. Energy spectra of these electrons are discussed.

Wang, J. R.↗
NASA NTRS1993

Measurements of Excitation Functions and Line Polarizations for Electron Impact Excitation of the n = 2, 3 States of Atomic Hydrogen in the Energy Range 11 - 2000 eV

The electron-atomic hydrogen scattering system is an important testing ground for theoretical models and has received a great deal of attention from experimentalists and theoreticians alike over the years. A complete description of the excitation process requires a knowledge of many different parameters, and experimental measurements of these parameters have been performed in various laboratories around the world. As far as total cross section data are concerned it has been noted that the discrepancy between the data of Long et al. and Williams for n = 2 excitations needs to be resolved in the interests of any further refinement of theory. We report new measurements of total cross sections and atomic line polarizations for both n=2 and n=3 excitations at energies from threshold to 2000 eV...

James, G. K.↗
NASA NTRS1974

OSO-7 observations of solar X-rays in the energy range 10-100 keV

Data on 123 hard X-ray bursts observed by the satellite OSO-7 between Oct. 10, 1971 and June 6, 1972 are described and evaluated. Typical duration of a burst is 100 sec. Average spectral indices lie between 3.5 and 5.5 for two-thirds of the 123 bursts, with a median of 4.6. In some events a soft-hard-soft pattern is observed, but there are numerous examples in which the spectrum softens continuously throughout the burst. The mean shape of the hard X-ray time profile as measured by the full width at half maximum does not depend on burst amplitude; nor does the spectral hardness correlate with the flux. The distribution of burst peak fluxes and the observation of large soft X-ray bursts without accompanying hard X rays suggest the existence of a distinct class of solar flares which emit only soft X rays. No center-to-limb variation was found in the frequency of occurrence of bursts or in the fraction with a nonthermal component. Estimates of the energy in the form of nonthermal electrons and in the flare plasma derived from these data indicate that the total amounts in each are comparable.

Datlowe, D. W.↗
DOE OSTI2020

Role of Spin–Orbit Coupling in Long Range Energy Transfer in Metal–Organic Frameworks

Metal–organic frameworks (MOFs) are emerging as a promising platform for solar energy conversion applications. Their potential utilization as efficient chromophores in artificial photosynthesis is closely related to the understanding of light-harvesting and energy transfer processes that occur within these molecular scaffolds. Herein, we present the photophysical investigation of Ru(II), Ir(III), and Os(II) polypyridyl complexes incorporated into the backbone of UiO-67. In this work, we systematically study the effect of spin–orbit coupling on dipole–dipole energy transfer in MOFs using steady-state and time-resolved spectroscopic techniques. The results of our work indicate successful triplet-to-singlet energy transfer and a sizable increase in the transfer kinetics and critical distance, as direct consequences of strong spin–orbit couplings. Remarkably, the reported R 0 value for OsDCBPY (R 0 = 88 ± 10 Å) represents one of the largest Förster distances observed in an MOF. Collectively, this work contributes to the general knowledge of energy transfer in materials and provides groundwork for efficient utilization in artificial photosynthetic assemblies.

37 INORGANIC, ORGANIC, PHYSICAL, AND ANALYTICAL CH↗