SEARCH · Engineering Papers
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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Evolution of 9 solar masses stellar model of population I initial composition from main sequence through core helium burning
Red shifts of quasi-stellar objects and relation to radio and optical magnitudes, concluding that red shifts have no relation to distance
Dynamics of ionized stellar winds noting anisotropic effect of stress tensors and densities, velocities and electrostatic potentials distributions
The Danish microsatellite, sted, is equipped with an autonomous, advanced stellar compass (ASC). The ASC consists of two separate units, a Charge Coupled Device (CCD) camera head (based on a commercial Sony interline CCD detector) and a data processing unit with a powerful microcomputer (Intel 80486 type processor). The microcomputer memory contains a star catalogue which enables the microcomputer to recognize the constellations of stars in the field of vies and thus derive the attitude of the ASC camera head. The mission, and the design, operation and performance of the ASC are described. Results of the ASC prototype tests at the Jet Propulsion Laboratory (JPL) Table Mountain Observatory (TMO) facility are given.
The formation of extremely hot outer atmospheres is one of the most prominent manifestations of magnetic activity common to late-type dwarf stars, including the Sun. It is widely believed that these atmospheric layers, the corona, transition region, and chromosphere, are heated by the dissipation of energy transported upwards from the stellar surface by the magnetic field. This is signified by the spectral line fluxes at various wavelengths, scaled with power-law relationships against the surface magnetic flux over a wide range of formation temperatures, which are universal to the Sun and Sunlike stars of different ages and activity levels. This study describes a catalog of power-law indices between solar activity proxies and various spectral line fluxes. Compared to previous studies, we expanded the number of proxies, which now includes the total magnetic flux, total sunspot number, total sunspot area, and the F10.7 cm radio flux, and further enhanced the number of spectral lines by a factor of 2. This provides the data to study in detail the flux–flux scaling laws from the regions specified by the temperatures of the corona (log(T/K) = 6–7) to those of the chromosphere (log(T/K) ∼ 4), as well as the reconstruction of various spectral line fluxes of the Sun in the past, F-, G-, and K-type dwarfs, and the modeled stars.
Stellar spectrophotometry from above the atmosphere
Study of planetary atmospheres by stellar occultation
Atmospheric sounding by satellite measurements of stellar refraction
Stellar spectrum lines - formation and intensity
Test for the verification of the dynamo theory of earth and stellar magnetism
Stellar spectra and ultraviolet auroral observations by aerobee rockets in the 1,300-1,800 angstrom region
Ultraviolet aurora with north-south asymmetry and stellar spectra taken from aerobee rocket flight
Distribution of meteors according to stellar magnitude
Comments on huang theory of probability of planet position near a star and on the location of stellar life zones
Termination of proton-proton chain in stellar interiors, noting influence of deuterium and helium 3 burning reactions
Relationship between chemical composition and photometric metal index in stellar atmospheres