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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 415 records · Page 23
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NASA NTRS1982

Mass flow due to heating in a binary system - Application to U Cephei

The possibility of mass flow due to the heating of the cooler component in a close binary system has been investigated. The heating may be caused by irradiation from the hotter companion or by other mechanisms such as the spacial coincidence of non-linear 'g-mode' oscillations in the cooler star. The 2.4-day period binary U Cep, in which gas streaming has been observed, has been chosen for model calculations. Preliminary results show that such a heating of the lower atmosphere of the cooler star could lead to mass flow at an average rate of 10 to the -9th - 10 to the -7th solar mass per year without the star necessarily filling its critical Roche surface.

Kondo, Y.↗
NASA NTRS1982

Planetary-scale waves in the Venus atmosphere

Observed wave-like cloud features on Venus, which at times form a Y-like structure which encircles the planet, were modelled numerically. Linearized primitive equations for a shallow, hydrostatic atmosphere are defined, along with upper boundary layer conditions for the 4-6 day periods detected in the atmospheric response to forcing. The basic state of the Venus atmosphere was considered to display variations in static stability and the mean zonal wind as a function of altitude. Forcing was introduced over a wide range of frequencies in order to produce the target oscillation modes. Combination of a midlatitude Rossby wave and an equatorial Kelvin wave was found to yield the observed Y-shape, which could be preserved with nonlinear coupling.

Covey, C.↗
NASA NTRS1984

Attempt to measure the solar subsurface velocity

Five-minute oscillation modes are advected by horizontal velocities below the solar surface, and thus can be used as probes of rotation and large-scale convective flows. Results of inverse theory applied to observations of high-degree modes carried out on six separate days reveal variations in horizontal velocities with depth from day to day that may be the result of giant convection cells, through noise in the data makes this interpretation somewhat tentative.

Hill, F.↗
NASA NTRS1984

The Fourier Tachometer 2: an Instrument for Measuring Global Solar Velocity Fields

The High Altitude Observatory and Sacramento Peak Observatory have jointly constructed a second version of the Fourier Tachometer, which is now undergoing final integration and testing. This is an interferometric instrument for measuring the Doppler shift of solar spectrum lines. The principal features and performance goals of this instrument are: simultaneous velocity observations over a 2-dimensional, 100 x 100 pixel field of view; measurement of absolute Doppler shifts with 1 m/s accuracy; noise level for moderate-1 oscillation modes of 1 cm/s for a 1-day observing run; flexibility and ease of use. Early (though incomplete) testing suggests that these goals should be attainable with the current instrument.

Brown, T. M.↗
NASA NTRS1985

A unified theory of coronal heating

Solar coronal heating mechanisms are analyzed within the framework of a unified theory of heating processes. The theory is based on the standing wave equation of Ionson (1982) for the global current driven by emfs from the convection Beta less than 1. The equation has the same form as a driven LRC equation in which the equivalent inductance is scaled with the coronal loop length. The theory is used to classify various heating mechanisms inside the coronal loops. It is shown that the total global current can be obtained from an integration of the local currents, the degree of coherency between local currents being the dominant factor governing the global current amplitude. Active region loops appear to be heated by electrodynamic coupling to p-mode oscillations in the convection Beta less than 1.

Ionson, J. A.↗
NASA NTRS1986

Dayside pulsation events near the plasmapause

Magnetic field observations of four dayside pulsation events detected near the equatorial plasmapause region on August 23, 24, September 30, and October 10, 1982 are examined. The wave characteristics and the magnetic components of the pulsation events obtained from DE-1 satellite data and ground data from Siple, Antarctica are described and compared. The pulsations displayed similar complex wave structures; long period transverse waves greater than 100 s are the fundamental mode oscillations of magnetic shells and short period waves of 20-40 s are superimposed on them. It is observed that wave bursts are present in all frequency ranges. The relationship between eigenperiod and the magnetic shell is studied.

Lin, N. G.↗
NASA NTRS1986

Motions in the interiors and atmospheres of Jupiter and Saturn. II - Barotropic instabilities and normal modes of an adiabatic planet

A rotating and adiabatic inviscid fluid planet possesses low frequency motions that are barotropic, quasi-geostrophic and quasi-columnar. The limiting curvature at which flow becomes unstable upon projection onto the planetary surface is negative, with an amplitude that is 3-4 times that for thin atmospheres, in planets in which density linearly decreases to zero at the surface. This result is shown to hold for all quasi-columnar perturbations. Both the phase speed of the normal mode oscillations and the barotropic stability criterion have features in common with Saturn and Jupiter oscillations.

Ingersoll, A. P.↗
NASA NTRS1986

Effects of fibril magnetic fields on solar p-modes. II - Calculation of mode frequency shifts

The effect of magnetic flux tubes in the solar convection zone on p-mode oscillations is investigated analytically using WKB ray theory, extending the results of Bogdan and Zweibel (1985) to the case of propagation not perpendicular to the tubes. Results for the frequency shift in polytropic slabs with vertical or horizontal flux tubes are presented in graphs and discussed.

Zweibel, E. G.↗
NASA NTRS1987

Simultaneous measurements of sunspot umbral oscillations in the photosphere, chromosphere, and transition region

Measurements of umbral oscillations in a sunspot were made simultaneously from space (with the SMM/UVSP instrument) in the C IV transition-region line and from the ground (with the tower telescope at NSO/sunspot) in spectral lines formed in the photosphere and chromosphere. The power spectra of velocity and intensity variations show multiple peaks in the 3 min band (4.5-10 mHz). A strong oscillation at 5.5 mHz is coherent between the chromosphere and transition region. Another strong oscillation mode at 7.5 mHz is coherent between the photosphere and transition region and appears to have a node in the chromosphere. The rms velocity in the 3 min band is a little over 12 km/sec in both the chromosphere and transition region, but the kinetic energy density is lower in the transition region (by a factor of 10 or more) due to the lower mass density there. These measurements of amplitude and phase of the waves at different heights provided a new, independent method of testing or fitting models of the vertical temperature distribution in the umbral chromosphere and transition regions.

Thomas, John H.↗
NASA NTRS1987

Theoretical investigations of X-ray bursts

Current theoretical understanding of the X-ray burst phenomenon is reviewed, providing a framework in which the burst radiation can be used as a diagnostic of the fundamental properties of the underlying neutron star. The typical Type I X-ray burst is detected as a rapid increase in emission to a level about a factor of 10 above that seen during the quiescent state and recurs on time scales which range from several hours to several days. The thermonuclear flash model has successfully reproduced the basic features of the X-ray burst phenomenon and thereby provided strong theoretical evidence that neutron stars are involved. Topics covered include: theory of the emission spectrum; oscillation modes and prospects for diagnosing the thermal state of neutron stars through experiments on board the X-Ray Timing Explorer or the Advanced X-Ray Astrophysics Facility; applications to the mass and radius of a neutron star.

Taam, Ronald E.↗
NASA NTRS1987

The 152-day periodicity of the solar flare occurrence rate

The occurrence rate of solar flares exhibits a periodicity of about 152 days. The cause of the 152-day periodicity still remains a mystery. But answers to the following questions will enhance understanding of it. (1) Is the periodicity a local or a global phenomenon? (2) Is the periodicity due to the interaction of 'hotspots' rotating at different rates such that they align with one another once every 152-day period? (3) Is the periodicity due to the interaction of rotating features originating from g-mode oscillations? Here the authors report an analysis of 'major flares' observed with the Hard X-ray Burst Spectrometer (HXRBS) aboard SMM and conclude that the 152-day periodicity is a global phenomenon, and that the answers to questions (2) and (3) are negative.

Bai, Taeil↗
NASA NTRS1987

Sunspot observations from the SOUP instrument on Spacelab 2

A series of white light images obtained by the SOUP instrument on Spacelab 2 of active region 4682 on August 5, 1985 were analyzed in the area containing sunspots. Although the umbra of the spot is underexposed, the film is well exposed in the penumbral regions. These data were digitally processed to remove noise and to separate p-mode oscillations from low velocity material motions. The results of this preliminary investigation include: (1) proper motion measurements of a radial outflow in the photospheric granulation pattern just outside the penumbra; (2) discovery of occasional bright structures (streakers) that appear to be ejected outward from the penumbra; (3) broad dark clouds moving outward in the penumbra in addition to the well known bright penumbral grains moving inward; (4) apparent extensions and contractions of penumbral filaments over the photosphere; and (5) observation of a faint bubble or loop-like structure which seems to expand from two bright penumbral filaments into the photosphere.

Shine, R. A.↗
NASA NTRS1987

Uniform period spacings in white dwarf models

Theoretical models of g-mode oscillations in white dwarfs are investigated analytically. Numerical results of period-spacing computations for DOV, DAV, and DBV models are presented in tables, and the relationships between period spacings and the composition and structure of the stellar atmospheres are discussed.

Kawaler, Steven D.↗
NASA NTRS1988

Stability of radiative shocks with time-dependent cooling

A full evolutionary calculation of ion abundances and radiative cooling has been incorporated into an accurate one-dimensional gasdynamics calculation in order to investigate the dynamics of radiative shock instability and to determine the extent to which power-law cooling models describe the situation. Radiative shocks are shown to be unstable for velocities of greater than about 140 km/s. The temperature dependence of cooling functions behind steady shocks suggests that the stability limit may depend upon the amplitude of the perturbation. Oscillation is noted in the fundamental oscillation mode.

Gaetz, T. J.↗
NASA NTRS1988

Solar models, neutrino experiments, and helioseismology

The event rates and their recognized uncertainties are calculated for 11 solar neutrino experiments using accurate solar models. These models are also used to evaluate the frequency spectrum of the p and g oscillations modes of the sun. It is shown that the discrepancy between the predicted and observed event rates in the Cl-37 and Kamiokande II experiments cannot be explained by a 'likely' fluctuation in input parameters with the best estimates and uncertainties given in the present study. It is suggested that, whatever the correct solution to the solar neutrino problem, it is unlikely to be a 'trival' error.

Bahcall, John N.↗
NASA NTRS1988

Observations on the dynamics of electromagnetically levitated liquid metals and alloys at elevated temperatures

Electromagnetic levitation and heating of small (0.5 to 1.0 gm) samples of Cu, Ni, and Ni-base alloys were performed in inert atmospheres. These experiments were recorded by high-speed photography using both regular film and video methods. Initial studies revealed interesting dynamics of the droplets that included axisymmetric oscillation, rotation, and oscillation mode changes. An attempt is made to explain the behavior using available models.

Hansen, G. P.↗
NASA NTRS1988

Radial and latitudinal gradients in the solar internal angular velocity

The frequency splittings of intermediate-degree (3 to 170 deg) p-mode oscillations obtained from a 16-day subset of observations were analyzed. Results show evidence for both radial and latitudinal gradients in the solar internal angular velocity. From 0.6 to 0.95 solar radii, the solar internal angular velocity increases systematically from 440 to 463 nHz, corresponding to a positive radial gradient of 66 nHz/solar radius for that portion of the solar interior. Analysis also indicates that the latitudinal differential rotation gradient which is seen at the solar surface persists throughout the convection zone, although there are indications that the differential rotation might disappear entirely below the base of the convection zone. The analysis was extended to include comparisons with additional observational studies and between earlier results and the results of additional inversions of several of the observational datasets. All the comparisons reinforce conclusions regarding the existence of radial and latitudinal gradients in the internal angular velocity.

Rhodes, Edward J., Jr.↗