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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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Discovery of a comet, 5 deg from the sun, during total eclipse of July 20th, 1963
Photographic tracking of comet during total solar eclipse
Douglas tasks for Airborne Solar Eclipse Expedition of May 30, 1965
Airborne scientific equipment procurement and installation aboard CV-990 aircraft for NASA SOLAR eclipse flight
Optical determination of temperature variations throughout the solar corona during the eclipse of May 30, 1965 Final report, 1 Feb. - 31 Jul. 1965
Optical determination of temperature variations throughout solar corona during eclipse of May 30, 1965
Use of the Moon to Distinguish the F from the K Corona Using a Rocket Coronagraph During an Eclipse
F and K corona observations by rocket coronagraph during solar eclipse
Ionospheric Electron Density During Solar Eclipse of 20 July 1963
Ionospheric electron density during solar eclipse
Eclipse will be photographed from space
Sounding rocket, satellite, and jet transport experiments for South American solar eclipse
Airplane stabilization and guidance for eclipse photography.
Aircraft stabilization for solar eclipse observation, emphasizing use of autopilot for maximum control
An Airborne Experiment to Determine Temperature Variations Throughout the Solar Corona During the Eclipse of 12 November 1966 Quarterly Status Report, 1 Oct. - 31 Dec. 1966
Airborne experiment to determine temperature variations throughout solar corona during eclipse of November 1966
Coronal photographs, isophotes, and a flash spectrum from the solar eclipse of May 30, 1965
Coronal photographs, isophotes, and flash spectrum from solar eclipse of 30 May, 1965
Radio spectrum of an active solar region determined from the 20 July 1963 eclipse.
Radio spectrum of active region near east limb of Sun determined from July 20, 1963 eclipse
Infrared emission during a simulated lunar eclipse.
IR emission measurement of lunar-like materials during simulated eclipse, noting dependence on time
Observations of the lunar eclipse of December 19, 1964, at a wavelength of 3.3 mm.
Radiometric observations of total lunar eclipse of December 19, 1964 at wavelength of 3.3 mm indicate no significant temperature difference
Temperature of the Solar Corona from Intensity Gradients Measured During the May 30, 1965 Total Eclipse
Solar corona temperature from intensity gradients measured during total eclipse of May 30, 1965
Temperature of the Solar Corona from Intensity Gradients Measured During the May 30, 1965 Total Eclipse
Corona temperature and logarithmic intensity gradients determined by pointwise three-color photoelectric photometry during solar eclipse
A Coordinated X-Ray and Optical Campaign of the Nearest Massive Eclipsing Binary, Delta Orionis Aa. I. Overview of the X-Ray Spectrum
We present an overview of four deep phase-constrained Chandra HETGS X-ray observations of Delta Ori A. Delta Ori A is actually a triple system that includes the nearest massive eclipsing spectroscopic binary, Delta Ori Aa, the only such object that can be observed with little phase-smearing with the Chandra gratings. Since the fainter star, Delta Ori Aa2, has a much lower X-ray luminosity than the brighter primary (Delta Ori Aa1), Delta Ori Aa provides a unique system with which to test the spatial distribution of the X-ray emitting gas around Delta Ori Aa1 via occultation by the photosphere of, and wind cavity around, the X-ray dark secondary. Here we discuss the X-ray spectrum and X-ray line profiles for the combined observation, having an exposure time of nearly 500 ks and covering nearly the entire binary orbit. The companion papers discuss the X-ray variability seen in the Chandra spectra, present new space-based photometry and ground-based radial velocities obtained simultaneously with the X-ray data to better constrain the system parameters, and model the effects of X-rays on the optical and UV spectra. We find that the X-ray emission is dominated by embedded wind shock emission from star Aa1, with little contribution from the tertiary star Ab or the shocked gas produced by the collision of the wind of Aa1 against the surface of Aa2. We find a similar temperature distribution to previous X-ray spectrum analyses. We also show that the line half-widths are about 0.3−0.5 times the terminal velocity of the wind of star Aa1. We find a strong anti-correlation between line widths and the line excitation energy, which suggests that longer-wavelength, lower-temperature lines form farther out in the wind. Our analysis also indicates that the ratio of the intensities of the strong and weak lines of Fe XVII and Ne X are inconsistent with model predictions, which may be an effect of resonance scattering.
The Ionospheric Three-Dimensional Electron Density Variations Induced by the 21 August 2017 Total Solar Eclipse by Using Global Ionospheric Specification
Global Ionospheric Specification (GIS) is based on the Gauss–Markov Kalman filter to assimilate the slant total electron content (TEC) observed from ground-based GPS receivers and space-based radio occultation instrumentations in order to reconstruct three-dimensional (3D) ionospheric electron density structure, and it can remotely sense and monitor the weather condition in space. In this study, five minutes of high temporal resolution GIS is implemented in order to reconstruct the 3D electron density structure on the 21 August 2017 total solar eclipse and analyze the variations induced by the moon’s shadow. To obtain more information of the ionosphere, from the extend 2200 GPS stations on the continental United States, are added for assimilation. The results show the ionosphere peak height (hmF2) uplift was 30–50 km altitude in latitude 25–40°N, and that the electron density depletion at higher altitudes (400 km) has a more noticeable time delay than at low altitudes (200 km), especially in low-latitude regions.
A Glimpse of the Solar Eclipse from NREL
On August 21, the NREL campus in Golden, Colorado experience a near-complete eclipse of the sun. This video, recorded from NREL’s Solar Radiation Research Laboratory, where researchers carefully measure the sun’s energy, captures the moon crossing the sun before clouds move in and cover the sun.