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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 1,747 records · Page 97
All sourcesNASA NTRSDOE OSTI
DOE OSTI2018

Enhancing the x-ray output of a single-wire explosion with a gas-puff based plasma opening switch

Here, we present experiments performed on the 1 MA COBRA generator using a low density, annular, gas-puff z-pinch implosion as an opening switch to rapidly transfer a current pulse into a single metal wire on axis. This gas-puff on axial wire configuration was studied for its promise as an opening switch and as a means of enhancing the x-ray output of the wire. We demonstrate that current can be switched from the gas-puff plasma into the wire, and that the timing of the switch can be controlled by the gas-puff plenum backing pressure. X-ray detector measurements indicate that for low plenum pressure Kr or Xe shots with a copper wire, this configuration can offer a significant enhancement in the peak intensity and temporal distribution of radiation in the 1–10 keV range.

70 PLASMA PHYSICS AND FUSION TECHNOLOGY↗
DOE OSTI2012

BLISTERING AND EXPLOSIVE DESORPTION OF IRRADIATED AMMONIA-WATER MIXTURES

We present laboratory studies on the thermal evolution of a solid ammonia-water mixture after it has been irradiated at 20, 70, and 120 K. In samples irradiated at {<=}70 K, we observed fast outbursts that appear to indicate grain ejection and correlate well with the formation of micron-sized scattering centers. The occurrence of this phenomenon at the lower irradiation temperatures indicates that our results may be most relevant for understanding the release of gas and grains by comets and the surfaces of some of the colder icy satellites. We observe outgassing at temperatures below those where ice sublimates, which suggests that comets containing radiolyzed material may have outbursts farther from the Sun that those that are passive. In addition, the estimated size of the grains ejected from our sample is on the order of the size of E-ring particles, suggesting that our results give a plausible mechanism for how micron-sized grains could be formed from an icy surface. Finally, we propose that the presence of the {approx}4.5 {mu}m N{sub 2}O absorption band on an icy surface in outer space will serve to provide indirect evidence for radiation-processed ices that originally contained ammonia or nitrogen, which could be particularly useful since nitrogen is such a weak absorber in the infrared and ammonia is rapidly decomposed by radiolysis.

79 ASTRONOMY AND ASTROPHYSICS↗
DOE OSTI2015

AM Canum Venaticorum progenitors with helium star donors and the resultant explosions

We explore the outcome of mass transfer via Roche lobe overflow of M{sub He}≲0.51M{sub ⊙} pure helium burning stars in close binaries with WDs. The evolution is driven by the loss of angular momentum through gravitational wave radiation (GWR), and both stars are modeled using Modules for Experiments in Stellar Astrophysics (MESA). The donors have masses of M{sub He}=0.35,0.4,and0.51M{sub ⊙} and accrete onto WDs of mass M{sub WD} from 0.6M{sub ⊙} to 1.26M{sub ⊙}. The initial orbital periods (P{sub orb}) span 20–80 minutes. For all cases, the accretion rate onto the WD is below the stable helium burning range, leading to accumulation of helium followed by unstable ignition. The mass of the convective core in the donors is small enough so that the WD accretes enough helium-rich matter to undergo a thermonuclear runaway in the helium shell before any carbon–oxygen enriched matter is transferred. The mass of the accumulated helium shell depends on M{sub WD} and the accretion rate. We show that for M{sub He}≳0.4M{sub ⊙} and M{sub WD}≳0.8M{sub ⊙}, the first flash is likely vigorous enough to trigger a detonation in the helium layer. These thermonuclear runaways may be observed as either faint and fast Ia SNe or, if the carbon in the core is also detonated, Type Ia SNe. Those that survive the first flash and eject mass will have a temporary increase in orbital separation, but GWR drives the donor back into contact, resuming mass transfer and triggering several subsequent weaker flashes.

79 ASTRONOMY AND ASTROPHYSICS↗