Periodic excitation of multiple-unit impact dampers
Steady state motion equations of multiple unit impact damper attached to periodically excited primary system, developing solution for mathematical model
Masri, S. F.↗
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Results for “equation of state”
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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Stellar structure theory
Stellar structure theory, examining particle aggregates gravitational and pressure forces, energy flow, generation and opacity and equations of state
Iben, I., Jr.↗
Partition functions in ionizing plasmas
Ionizing plasmas partition functions, determining opacities and equations of state
Fischel, D.↗
Neutron star models including the effects of hyperon formation
Neutron star matter equations of state involving hyperon formation effects for maximal stable mass models, tabulating moments of inertia
Cameron, A. G. W.↗
Convective transport of low energy cosmic rays in the interplanetary region
Cosmic ray propagation in interplanetary space, deriving steady state transport equation with energy losses
Gleeson, L. J.↗
Spectral factorization in time-varying systems having periodic coefficients and its application to navigation of solar electric interplanetary missions
Low thrust interplanetary spacecraft tracking, using spectral factorization for Kalman filtering equations steady state solution
Nishimura, T.↗
Joule-Thomson inversion curves and related coefficients for several simple fluids
The equations of state (PVT relations) for methane, oxygen, argon, carbon dioxide, carbon monoxide, neon, hydrogen, and helium were used to establish Joule-Thomson inversion curves for each fluid. The principle of corresponding states was applied to the inversion curves, and a generalized inversion curve for fluids with small acentric factors was developed. The quantum fluids (neon, hydrogen, and helium) were excluded from the generalization, but available data for the fluids xenon and krypton were included. The critical isenthalpic Joule-Thomson coefficient mu sub c was determined; and a simplified approximation mu sub c approximates T sub c divided by 6P sub c was found adequate, where T sub c and P sub c are the temperature and pressure at the thermodynamic critical point. The maximum inversion temperatures were obtained from the second virial coefficient (maximum (B/T)).
Hendricks, R. C.↗
Examination of two methods of describing the thermodynamic properties of oxygen near the critical point
A computer study was conducted to compare the numerical behavior of two approaches to describing the thermodynamic properties of oxygen near the critical point. Data on the relative differences between values of specific heats at constant pressure (sub p) density, and isotherm and isochor derivatives of the equation of state are presented for selected supercritical pressures at temperatures in the range 100 to 300 K. The results of a more detailed study of the sub p representations afforded by the two methods are also presented.
Rees, T. H.↗
Interrelated structure of high altitude atmospheric profiles
A preliminary development of a mathematical model to compute probabilities of thermodynamic profiles is presented. The model assumes an exponential expression for pressure and utilizes the hydrostatic law and equation of state in the determination of density and temperature. It is shown that each thermodynamic variable can be factored into the produce of steady state and perturbation functions. The steady state functions have profiles similar to those of the 1962 standard atmosphere while the perturbation functions oscillate about 1. Limitations of the model and recommendations for future work are presented.
Engler, N. A.↗
Study of dense aluminum plasmas
Studies directed toward the development of a computer program describing the penetration of a thin aluminum plate by a quartz sphere are reported. The aluminum simulates a bumper plate for micrometeoroids. The ablation of a rock sphere by penetrating a stack of paper sheets is described, and an equation for losses near the surface of the sphere is derived. The expansions of aluminum plasma sphere with initial energies of 44.45, 20.8, and 7.136 eV are investigated, including shock compression during penetration and adiabatic expansion. The equations of state were derived for aluminum and quartz, as well as one of the Mie-Grunesen type. A technique to determine momentum at the bottom surface of the thin plate, and the energy for hypervelocity separation of fragments of the aluminum plate are also considered.
Todd, F. C.↗
The neutron star as a quantum crystal
The structure of the interior of neutron stars was examined. The equation of state for the interior of neutron stars was calculated.
Canuto, V. M.↗
More solar models and neutrino fluxes.
Derivation of neutrino fluxes from a sequence of solar models that differ from one another in regard to opacity, equation of state, and nuclear cross-section factors. Using current estimates of the relevant input parameters, capture rates are obtained that range between three and ten times the most recent result of the Davis Cl 37 neutrino-capture experiment. The contribution to a theoretical capture rate due to neutrinos from all reactions other than B 8 decay ranges from 0.5 to 1.5 times the latest observational result. Comparison with results of other solar model calculations indicates reasonable agreement when results are normalized to the same input parameters.
Abraham, Z.↗
Gasdynamics of explosions today.
A brief review is given of blast and detonation wave phenomena and some of their uses in war and peace. It is concluded that great strides have been made over the last three decades toward the physical understanding, the analytical-numerical solution, and the measurement of dynamic and thermodynamic quantities, also taking into consideration severe environments and extremely short durations. Questions of internal ballistics are discussed together with hypervelocity launchers and shock tubes, collapsing cylindrical drivers, spherical implosions, explosive weapons, dynamic response, and equation of state data.
Brode, H. L.↗
Solar wind for a magnetized plasma with tensor plasma pressure.
A solar wind model for a magnetized solar wind is presented using one-fluid hydromagnetic equations with generalized polytrope equations of state for the two tensor components of the plasma pressure. Fluid and magnetic field variables are calculated at the Earth using certain boundary conditions at the Sun. The azimuthal velocity agrees with observed values and explains the considerable loss of angular momentum from the Sun by the solar wind. The results are good for most variables but suggest that a two-fluid model with electrons at higher temperatures and smaller temperature anisotropy ratios than the ions would give improved agreement for some quantities.
Tan, M.↗
Attitude control of a spinning Skylab.
Active attitude control of a spinning Skylab is analyzed to determine a simple control law that will provide a satisfactory response, considering the dynamics of attached flexible appendages. A simplified model of the complex Skylab vehicle is selected to make it analytically tractable. The vehicle is modeled as a single rigid-core body with two attached flexible massless booms having masses on their tips. The equations of motion describing the attitude dynamics of the model are presented as a linear matrix-differential equation. The states of the vehicle are small perturbations about its steady-state spin. An analysis is performed to determine the domain of stability. Next, attitude dynamics are analyzed; both frequency domain (parameter plane) and time domain (an optimal linear quadratic loss program) techniques are compared. An analysis of the nonlinear effect of control torque saturation of Skylab's control moment gyroscopes is discussed. The results of the analysis compare favorably with a large-scale digital simulation of the Skylab.
Seltzer, S. M.↗
Surface composition of magnetic neutron stars.
The relative abundances of seven constituent nuclei, He4, C12, O16, Ne20, Mg24, Si28, and Fe56, are calculated as a function of time for neutron star atmospheres within which exist magnetic fields of the order of 10 to the 13th G. The opacity, equation of state of the electrons, and cooling rate of the magnetic star are discussed, and it is shown to be a reasonable approximation to assume an atmosphere to be isothermal. The effects of particle diffusion are included in the nuclear reaction network. Computations are performed both for a constant mass atmosphere and for an atmosphere in which mass is being ejected. It is found that the final abundances are model-independent, as long as the initial model contains predominantly He4. The relative abundances are compared to the cosmic ray spectrum. For both the constant-mass and mass-loss atmospheres, nucleosynthesis proceeds virtually completely to Fe56. However the outermost layers of the envelope, in which no mass is being ejected, are composed almost entirely of He4 with trace amounts of Fe56. After the loss of about 10 to the 21st g, only Fe56 is ejected from atmospheres expelling mass.
Rosen, L. C.↗
Minimum mass of a neutron star.
The equation of state at subnuclear densities is considered together with the average binding energy per nucleon and the possibilities for a conversion of a neutron star into a white dwarf. It is found that the stable minimum mass with a core of pure neutron gas is equal to 0.067 units in terms of the solar mass, and with a core clustered with heavy nuclei equals 0.093 units. The real minimum mass is probably somewhere between these two numbers.
Leung, Y. C.↗
Neutron stars.
Particular attention is given to the physical concepts underlying neutron stars. The characteristics of an equation of state which is suitable for a neutron star configuration are discussed. Cold neutron star models are examined, including the properties of a particular model in the intermediate range of stable models. Questions regarding the thermal energy of a neutron star are discussed together with aspects of vibrational energy, rotational energy, magnetic energy, and problems in connection with the Vela pulsar.
Cameron, A. G. W.↗