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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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Electromagnetic interactions in hyperfine structure of vibrational and rotational states in rubidium and potassium /isotopes/ fluorides, using electric resonance method
EPR observation of Eu ion transformation from trivalent to divalent charge states under illumination in cadmium fluoride-Eu crystal
Identification of faint emission Herzberg bands in oxygen-argon afterglow
Spin-lattice Hamiltonian for trivalent positive Nd and U ions in sites of tetragonal symmetry in calcium fluoride measured with electron spin resonance
Direct one phonon spin-lattice relaxation times for positive trivalent Nd and U ions in calcium difluoride at tetragonal symmetry sites
Helium I line profiles including forbidden component, discussing electron and ion Stark broadening and thermal Doppler broadening
Lithium 6 and 7 fission following pion capture, searching for H 4 and 5
Reaction rate constants of ion-molecule interchange reaction as function of temperature, flow velocity, activation energy and constant part of steric factor P
Leak rate measurement accuracy of rate-of-rise technique for nitrogen, methane and He between millionth and thousandth torr
Molecular N UV spectrum at various pressures, showing absorption band dependence on pressure induced dipole transitions
Cosmic ray origin in high energy H and He isotropic abundances and energy spectra observed by IMP 4 satellite during solar quiet times
A new high pedestal regime (“Super H-mode”) has been predicted and accessed on DIII-D. Super H-mode was first achieved on DIII-D using a quiescent H-mode edge, enabling a smooth trajectory through pedestal parameter space. By exploiting Super H-mode, it has been possible to access high pedestal pressures at high normalized densities. While elimination of Edge localized modes (ELMs) is beneficial for Super H-mode, it may not be a requirement, as recent experiments have maintained high pedestals with ELMs triggered by lithium granule injection. Simulations using TGLF for core transport and the EPED model for the pedestal find that ITER can benefit from the improved performance associated with Super H-mode, with increased values of fusion power and gain possible. Similar studies demonstrate that the Super H-mode pedestal can be advantageous for a steady-state power plant, by providing a path to increasing the bootstrap current while simultaneously reducing the demands on the core physics performance.
The riddle posed by super-Earths (1–4R{sub ⊕}, 2–20M{sub ⊕}) is that they are not Jupiters: their core masses are large enough to trigger runaway gas accretion, yet somehow super-Earths accreted atmospheres that weigh only a few percent of their total mass. We show that this puzzle is solved if super-Earths formed late, as the last vestiges of their parent gas disks were about to clear. This scenario would seem to present fine-tuning problems, but we show that there are none. Ambient gas densities can span many (in one case up to 9) orders of magnitude, and super-Earths can still robustly emerge after ∼0.1–1 Myr with percent-by-weight atmospheres. Super-Earth cores are naturally bred in gas-poor environments where gas dynamical friction has weakened sufficiently to allow constituent protocores to gravitationally stir one another and merge. So little gas is present at the time of core assembly that cores hardly migrate by disk torques: formation of super-Earths can be in situ. The basic picture—that close-in super-Earths form in a gas-poor (but not gas-empty) inner disk, fed continuously by gas that bleeds inward from a more massive outer disk—recalls the largely evacuated but still accreting inner cavities of transitional protoplanetary disks. We also address the inverse problem presented by super-puffs: an uncommon class of short-period planets seemingly too voluminous for their small masses (4–10R{sub ⊕}, 2–6M{sub ⊕}). Super-puffs most easily acquire their thick atmospheres as dust-free, rapidly cooling worlds outside ∼1 AU where nebular gas is colder, less dense, and therefore less opaque. Unlike super-Earths, which can form in situ, super-puffs probably migrated in to their current orbits; they are expected to form the outer links of mean-motion resonant chains, and to exhibit greater water content. We close by confronting observations and itemizing remaining questions.
The chiral conformal field theory of free super-bosons is generated by weight one currents whose mode algebra is the affinisation of an abelian Lie super-algebra h with non-degenerate super-symmetric pairing. The mode algebras of a single free boson and of a single pair of symplectic fermions arise for even|odd dimension 1|0 and 0|2 of h, respectively. In this paper, the representations of the untwisted mode algebra of free super-bosons are equipped with a tensor product, a braiding, and an associator. In the symplectic fermion case, i.e., if h is purely odd, the braided monoidal structure is extended to representations of the Z/2Z-twisted mode algebra. The tensor product is obtained by computing spaces of vertex operators. The braiding and associator are determined by explicit calculations from three- and four-point conformal blocks.
Force components of ion bombardment of copper & aluminum flat plates
Sputtering of meteorites by positive helium, neon, and argon ions
Second order forced nonlinear oscillation differential equation with time-dependent term not even, having infinity of periodic solutions
Potential curves for excited states of helium molecule computed from variational wave functions