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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 1,207 records · Page 67
All sourcesNASA NTRSDOE OSTI
NASA NTRS1979

The interstellar medium near the sun. II - The line of sight to Alpha Virginis

Measurements of the UV interstellar lines in Alpha Vir between 935 and 2960 A are reported. The derived abundances indicate significant depletion of Al, Si, Mn, Fe, and possibly Mg, whereas S, C, Ar, and O appear to be essentially undepleted. About half the gas is shown to be ionized, with a mean electron density of no more than 1 per cu cm, and the remainder is neutral, though both regions have the same velocity to within 2 km/s. A small fraction of the gas is apparently at a temperature of 400,000 K. The possibility of measuring the temperature of the H I gas is discussed, using the observed relationship between Doppler width and mass. A detailed discussion is included of the data analysis useful for comparatively simple lines of sight in terms of density, temperature, and extent of the possible physical regions, and of the relevant radiation field. An unidentified feature at 1063.2 A is reported.

York, D. G.↗
NASA NTRS1979

Evidence for large-scale velocity features on the sun

Giant velocity features on the solar surface are seen in line-of-sight velocity data from the Mount Wilson magnetograph. Velocity amplitudes around 40 m/s are seen in features with dimensions about 15 deg in latitude and 30-60 deg in longitude. These features are associated with solar activity. The largest such feature accompanied the largest complex of activity in this interval, lived for about 16 rotations, and predated the first magnetic fields in the area by about two rotations. A general pattern of upward motion at the equator is seen, and motions away from the earth at higher latitudes could represent a meridional flow toward the poles of the order of 20 m/s.

Howard, R.↗
NASA NTRS1978

Missions to the sun and to the earth

The program outlined in the present paper represents an optimized plan of solar terrestrial physics. It is constrained only in the sense that it involves not more than one new major mission per year for the Solar Terrestrial Division during the 1980-1985 period. However, the flight activity proposed, if accepted by the Agency and by Congress, would involve a growth in the existing Solar Terrestrial budget by more than a factor of 2. Thus, the program may be considered as somewhat optimistic when viewed in the broader context of the NASA goals and budget. The Agency's integrated FY 1980 Five Year Plan will show how many missions proposed will survive this planning process.

Timothy, A. F.↗
NASA NTRS1979

The observation and interpretation of the profile of C IV lambda-1548 emitted from a quiet region of the sun

The average properties of the quiet chromospheric network as seen in the transition region line of C IV at 1548 A have been investigated. Line profile data for the study were taken with the OSO 8 High Resolution Ultraviolet Spectrometer, which has moderate angular resolution, high spectral resolution, and good relative photometric accuracy. The profiles, when classified and averaged according to their intensities, were found to be symmetric and Gaussian in shape at all intensity levels. A marginally significant increase in line width with line intensity was detected but the average relative redshift in the network that has been a feature of other OSO 8 studies was not found. The network-to-cell contrast ratio was of the order of 13:1 with the extreme extending to 50.1. The measured average width of 0.22 A (FWHM) is in good agreement with earlier work. Finally, a theoretical interpretation is presented, based on both the line width measurement and consideration of the profile symmetry properties. It is concluded that acoustic waves alone cannot supply enough energy to balance the radiative and conductive losses from the corona. The data are, however, consistent with heating by Alfven waves.

Bruner, E. C., Jr.↗
NASA NTRS1979

Variation with time of a sun-weather effect

The reported influence (Wilcox et al., 1976) of the solar and interplanetary magnetic sector structure on terrestrial atmospheric vorticity at the 500 mbar level during the winters of 1963-1973 has been disputed by Williams and Gerety (1978). The present analysis indicates, however, that the response has been remarkably constant, if an apparent increase during the past few years in the intensity of tropospheric circulation is properly accounted for.

Wilcox, J. M.↗
NASA NTRS1980

Control of the Earth's electric field intensity through solar wind modulation of galactic cosmic radiation: Support for a proposed atmospheric electrical sun-weather mechanism

The ionospheric potential and galactic cosmic radiation, found to be inversely correlated with the solar wind velocity are examined as being germane to weather modification. Since the ionospheric potential is proportional to the fair weather electric field intensity and cosmic radiation is the dominant source of atmospheric ionization, it is concluded that the Earth's overall electric field varies in phase with atmospheric ionization and that the latter is modulated by the solar wind. A proposed mechanism, in which solar control of ionizing radiation influences atmospheric electrification and thus possibly cloud physical processes is discussed. An experimental approach to critically test the proposed mechanism through comparison of the temporal variation of the Earth's electric field with conditions in the interplanetary medium is outlined.

Markson, R.↗
NASA NTRS1980

The rotation of the Sun: Observations at Stanford

Daily observations of the photospheric rotation rate using the Doppler effect made at the Stanford Solar Observatory since May 1976 are analyzed. Results show that these observations show no daily or long period variations in the rotation rate that exceed the observational error of about one percent. The average rotation rate is the same as that of the sunspot and the large-scale magnetic field structures.

Scherrer, J. M.↗
NASA NTRS1980

Heat and electricity from the Sun using parabolic dish collector systems

Point focus distributed receiver solar thermal technology for the production of electric power and of industrial process heat is addressed. The thermal power systems project which emphasizes the development of cost effective systems which will accelerate the commercialization and industrialization of plants up to 10 MWe, using parabolic dish collectors is described. The projected size of the isolated load market in the 1990-2000 time period is 300 to 1000 MW/year. Although this market is small in comparison to the grid connected utility market, it is indicated that by assuming only a 20 percent market penetration, up to 10,000 power modules per year would be required to meet this need. At a production rate of 25,000 units/year and assuming no energy storage, levelized bus bar energy costs of 75 mills/kWeh are projected. These numbers are based on what is believed to be a conservative estimate regarding engine-generator conversion efficiency (40 percent) for the 1990 time period. With a more optimistic estimate of efficiency (i.e., 45 percent), the bus bar cost decreases to about 67 mills/kWeh. At very large production rates (400,000 modules/years), the costs decrease to 58 mills/kWeh. Finally, the present status of the technology development effort is discussed.

Truscello, V. C.↗
NASA NTRS1979

Heat and electricity from the sun using parabolic dish collector systems

The paper investigates point focus distributed receiver (PFDR) solar thermal technology for the production of electric power and of industrial process heat. Attention is given to a thermal systems project conducted by JPL under DOE sponsorship. It is reported that project emphasis is on the development of cost-effective systems which will accelerate the commercialization and industrialization of plants up to 10 MWe, using parabolic dish collectors. Also discussed are the characteristics of PFDR systems, the cost targets for major systems hardware, and markets for this technology. Finally, the present system status of the technology development effort is discussed.

Truscello, V. C.↗
NASA NTRS1980

The sun is observed to be a torsional oscillator with a period of 11 years

Twelve years of full-disk Mount Wilson velocity data have been analyzed to study horizontal east-west motions. A torsional wave pattern with alternating latitude zones of slow and fast rotation is found, after subtracting a differentially rotating frame. Amplitudes of the flow pattern average about 3 m/s. It requires about 22 years for zones to drift from the poles, where they originate, to the equator, where they disappear. The pattern is symmetric about the equator. The zones representing the next solar cycle (No. 22) are seen now at high solar latitudes. Solar active regions are formed in a latitude strip centered on the boundary of fast- and slow-velocity zones. This pattern evidently represents a deep-seated circulation pattern and is the first evidence of the association of mass motions with large-scale characteristics of the solar activity cycle.

Howard, R.↗
NASA NTRS1980

Life sciences: No place in the Sun

The status of the life sciences within NASA is reviewed. The historical movement towards a unified life sciences program is discussed.

Source record↗
NASA NTRS1981

The Sun as a star

Solar physics was reviewed in the context of the solar atmoshere. The understanding of the solar atmosphere is linked to stellar atmospheric research. Topics covered include: the existence of the chromosphere, the corona, and the solar wind; the interactive complex of convection, differential rotation, magnetic field generation and concentration, and the activity cycle; phenomena such as granulation, supergranulation, the 5 minute oscillation, filigree, faculae, sunspots, spicules, prominences, surges, and the spectacular flares.

Jordan, S. D.↗
NASA NTRS1981

The Sun as a star

The ways in which solar astrophysics serves to improve the methodology for the interpretation of stellar observations and the construction of stellar atmospheric models are summarized. The astrophysical processes highlighted are: stellar mass; stellar rotation; stellar magnetism; stellar composition; stellar companions; and evolutionary history.

Rutten, R. J.↗