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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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NASA NTRS1981

Observational, reference and model data on solar EUV, from measurements on AE-E

Information on solar irradiance at wavelengths below 185 nm, observed by the EUVS experiment on the AE-E satellite over the entire development of the present sunspot cycle 21, is important to a variety of investigations of planetary thermospheres and ionospheres. Since strictly observational information is generally lacking in both the completeness and the spectral detail required by the more advanced programs, it has been necessary to develop computer models in connection with fully detailed compilations of an appropriate reference spectrum. The period of July 13-18, 1976, is selected as an observationally reliable AE-E data reference period reflecting solar conditions of minimum activity for solar cycle 21. It is pointed out that the assignments of absolute irradiance-reference values have been drawn for all available sources of information other than that provided by AE-E.

Hinteregger, H. E.↗
NASA NTRS1982

Short-term EUV flux variations from AE-E He/+/ abundances

The ionization rate of helium in the thermosphere is inferred from AE-E ion and neutral particle composition measurements made on 20 days from January 1979 to June 1980. The variations in the inferred rate are consistent with variations in the UV flux measured during the same period by the AE-E UV spectrometer. The approximately 27-day modulation of the calculated ionization rate is the result of cyclical variations in the UV flux, which are in turn coupled to the rotation period of the sun. Results indicate that the ionization structure of helium in the thermosphere is closely coupled to both the long and short term EUV flux variations.

Sternberg, A.↗
NASA NTRS1982

EUV emission from Titan's upper atmosphere - Voyager 1 encounter

Most of the observed emission short of Lyman-alpha is shown to be accounted for by electron impact on N2 above 3600 km, in an analysis of Titan's EUV emission spectra obtained at the Voyager 1 encounter. It is determined that N2 is the major component of Titan's upper atmosphere, with 3900-km upper limit mixing ratios of NeI, ArI, CO, H2, and HI of 0.01, 0.06, 0.05, 0.06 and 0.1, respectively. Magnetospheric electron precipitation produces an average dayside electron density of about 3000/cu cm between 3600 and 4000 km, which is the region of bright limb emission, and magnetospheric electron impact dissociation of N2 generates an N atom escape rate of 3 x 10 to the 26th/sec from Titan's exosphere when Titan is within Saturn's magnetosphere.

Strobel, D. F.↗
NASA NTRS1983

The Saturn spectrum in the EUV - Electron excited hydrogen

Recent laboratory observations of electron excited H2 in the EUV have brought about the realization that higher Rydberg series band systems make a significant contribution to the emission spectrum. Theoretical cross section estimates for the excitation of the D, D-prime, B-prime, and B-double-prime states agree with these results. Model calculations for particle excitation of the Saturn atmosphere, including the higher states, now show excellent agreement with Voyager auroral and dayside equatorial spectra. The model data also confirm the relative spectral response calibration of the Voyager instruments, providing a basis for accurate analysis of the excitation processes on both Jupiter and Saturn.

Shemansky, D. E.↗
NASA NTRS1983

EUV branching ratios for ionized nitrogen and oxygen emissions

Branching ratios of single ionized atomic nitrogen and oxygen EUV emissions that terminate on the metastable states of the respective ions are presented. The four NII ratios and the 482/515 A ratio in OII reported represent the first measured values. Details of the wavelength calibration procedures adopted and a brief discussion of two modeling implications of the measured ratios are included.

Morrison, M. D.↗
NASA NTRS1983

The role of spicules in hetaing the solar atmosphere Implications of EUV observations

Although spicules hae been obseved for many years, very little is known about their role in the transport of mass and energy between the chromosphere and the higher layers of the atmospere. Athay and Holzer (1982) demonstrated that the rise and fall of spicular material can supply the thermal energy required for heating the upper chromosphere, transition, and possibly corona. The proposed mechanism depends upon assumptions about the fate of spicules after they disappear from view in the visual spectrum where observations are limited to spectral lines formed at chromospheric temperatures. The present investigation is concerned with an analysis of meaurements of the spatial and temporal variations of EUV emission near the solar limb. The obtained results place empirical constraints on the fate of spicules after they disappear from view in the visible spectrum and thereby place constraints on their role in the transport of mass and energy between the chromosphere and corona.

Withbroe, G. L.↗
NASA NTRS1983

O I (7990 A) emission and radiative entrapment of auroral EUV

The auroral O I 7990-A multiplet intensity distribution has been observed by means of a 2-m grille spectrometer and a Fabry-Perot interferometer during 1977 and 1982, respectively, in Alaska. Grille spectrometer results indicate a nonstatistical distribution in the excited state, consistent with the preferential scattering of the O I 989-A EUV emission and in accord with recent radiative transfer calculations. A comparison of O I 7990-A intensities measured on the nightside with those from dayside magnetospheric cleft aurora shows a cascade contribution to the O I 8446-A line, and ultimately to the O I 1304-A transition, that depends on the altitude of the aurora. This is attributed to the greater radiative enhancement of O I 989-A at low altitude, and the correspondingly enhanced probability for branching from the 3 s-prime to the 3 p level in atomic O.

Christensen, A. B.↗
NASA NTRS1982

Solar EUV, XUV and soft X-ray telescope facilities

Facility class, high resolution instrumentation can enable maximum spatial, spectral and temporal resolutions and provide understanding of the complex physical conditions in the outer solar atmosphere and the mechanisms responsible for these conditions. The scientific rationale for facility class instruments operating in the EUV, XUV, and soft X ray spectral ranges are discussed. Possible configurations for these facilities and priorities for their development are considered.

Withbroe, G. L.↗
NASA NTRS1984

Comparative lifetesting results for microchannel plates in windowless EUV photon detectors

Microchannel plates (MCPs) from seven manufacturers were subjected to a series of tests to determine their suitability for the Extreme Ultraviolet Explorer satellite. Comparative data are presented for sixteen MCP tandem pairs with channel length to diameter ratios (l/d) ranging from 40:1 to 60:1 and for two saturable (curved channel) MCPs with l/d's of 80:1. Results for MCPs with funnelled channel throats are also discussed. Properties of the MCPs which were monitored include: background count rate, output charge pulse height distribution (PHD), modal gain, PHD full width half maximum (FWHM), and extreme ultraviolet (EUV) photon quantum efficiency. Five detectors were chosen for further lifetime testing consisting of a mild bake to 100 C, and charge extraction to 0.01 coulombs, repeated high voltage cycling and reexposure to one atmosphere conditions. The results of these tests and their implications for the flight detectors are discussed. Erratic events in the detector background were recorded, probably due to field emission from high voltage surfaces or the absorption of water vapor into the electrode following exposure to air. The steps taken to control the detector background are discussed.

Malina, R. F.↗
NASA NTRS1984

A preliminary estimate of the EUVE cumulative distribution of exposure time on the unit sphere

A preliminary study of an all-sky coverage of the EUVE mission is given. Algorithms are provided to compute the exposure of the celestial sphere under the spinning telescopes, taking into account that during part of the exposure time the telescopes are blocked by the earth. The algorithms are used to give an estimate of exposure time at different ecliptic latitudes as a function of the angle of field of view of the telescope. Sample coverage patterns are also given for a 6-month mission.

Tang, C. C. H.↗
NASA NTRS1984

Line width of the solar EUV He I resonance emissions at 584 and 537 A

Instrumentation was carried aloft on a Black Brant rocket in August 1982 to gather spectrometry on the solar He I resonance lines. The payload consisted of a He spectrometer which furnished 11 readings at FWHM of close to 97 and 132 mA for the 584 and 537 a lines, respectively. The results indicated a variation of the solar line width that was inversely correlated with solar activity and with the solar EUV flux. Further studies of the 522 A line are recommended to detect any unidentified first order solar emissions close to or within the absorption profile of the 537 A line that contributed to the observed line width.

Ogawa, H. S.↗
NASA NTRS1984

Voyager EUV and FUV Observations

The Voyager 1 and 2 ultraviolet spectrometers are sensitive over the wavelength range 500 to 1700 A. In the extreme ultraviolet (EUV), at wavelengths shortward of the Lyman limit (912 A), Voyager observations detected emission from three out of a sample of 11 nearly hot DA white dwarfs. These observations imply very low HI column densities in the directions of the three stars detected. In the far ultraviolet (FUV), at wavelengths between 912 and 1200 A, Voyager observations of O and B stars can be used to study interstellar reddening at the shortest wavelengths and to provide useful estimates of interstellar H2 column densities.

Holberg, J. B.↗
NASA NTRS1984

Measuring EUV Line Emission from the Hot Interstellar Medium

In the local interstellar medium, the presence of hot gas was inferred from measurements of oxygen VI absorption in the ultraviolet, and from diffuse emission in the extreme ultraviolet (EUV) and soft X-ray regions. A spectrometer that is very sensitive to gas in this temperature range is described. The spectrometer uses an array of plane ruled gratings at grazing incidence in the extreme off plane mount. A set of Kirkpatrick-Baez mirrors focuses the conically diffracted light on to one of two microchannel plate detectors. The field of view of the instrument is 0.2 deg by 12 deg. The predicted sensitivity ranges from 50 to 200 ph/(sq cm sec str) with a resolving power of 15 to 50 over the 50 to 700 angstrom wavelength band.

Labov, S.↗
NASA NTRS1984

The evaluation of a deformable diffraction grating for a stigmatic EUV spectroheliometer

A second toroidal replica grating was found to have an aspect ratio within 10% of the desire value. The aspect ratio of replica toroidal gratings is coming out somewhat low. Whether this is caused by some relaxation in the epoxy or some residual error in the setup when the replication is made from the deformable submaster grating will be determined. The first imaging tests at EUV wavelengths near 500 A were carried out. The initial results are most encouraging with blur sizes of the order of, or less than, 40 microns. Further focussing and additional photographic tests will be carried out, and preparations made for the first photoelectric measurements of the image quality using the (256 x 1024)-pixel MAMA detection system. The visible-light (256 x 1024)-pixel MAMA detector tube has completed initial evaluation.

Timothy, J. G.↗
NASA NTRS1984

EUV airglow during active solar conditions. II - Emission between 530 and 930 A

Instrumentation on the Astrobee F sounding rocket on June 27, 1980 gathered EUV airglow data in the 530-930 A range. The 2-4 A resolution data were examined specifically for O II emission lines below 800 A, which were centered at 537-539 A. The emision was attributed to doublet and quartet components and exhibited a branching ratio of 3. A separate identification was made of O II emissions at 581 A. Inclusion of the 2s2p(4)2P state is therefore recommended in photoinization models of cometry and planetary atmospheres.

Gentieu, E. P.↗
NASA NTRS1984

The EUV spectrum of H2O by electron impact

The vacuum ultraviolet (VUV) spectrum of H2O produced by electron impact at 200 eV is presented. A total of 25 spectral features are identified at a resolution of 0.5 nm over the wavelength range from 40 to 280 nm. Absolute emission cross-sections were obtained for each of the features. The differences of the features are all attributed to the various excited states of the dissociation products, H, O and O(+). The Lyman-alpha feature is the brightest for electron-induced fluorescence of H2O from the UV to the near-IR, and had a cross-section of 6.3 (+ or - 1.0 x 10 to the -18th) sq cm at 200 eV. The Lyman-alpha feature contributed 74 percent of the total measured emission cross-section in the EUV.

Ajello, J. M.↗
NASA NTRS1986

The implication for the presence of a magnetosphere on Uranus in the relationship of EUV and radio emission

A report by Kaiser and Desch (1985) indicates that nonthermal radio emissions from Uranus were not detectable from the Voyager spacecraft at a range of less than 0.7 AU. This observation suggests that the planet may have significantly different magnetospheric characteristics than Jupiter and Saturn. The ratio of atomic to molecular emission in the hydrogenic atmospheres of the outer planets varies over a wide range depending on the nature of the exciting process and the altitude of the sources. The importance of the ratio of atomic to molecular emission is discussed along with the escape of atomic hydrogen. On the basis of an evaluation of the observations, the possibility is raised that the strong EUV radiation from Uranus may not be auroral in origin.

Shemansky, D. E.↗
NASA NTRS1986

A simple technique for estimating EUVE sky survey exposure times

A simple way to estimate accumulated exposure time over the celestial sphere for a scanning telescope in earth orbit is described. Primary constraints on observation time, such as earth blockage, solar occultation, and passage through the South Atlantic Anomaly, are modeled using relatively straightforward, mainly closed-form geometrical solutions. The resulting algorithm is implemented on a desktop microcomputer. Though not rigorously precise, the algorithm is sufficient for conducting preliminary mission design studies for the Extreme Ultraviolet Explorer (EUVE).

Carlisle, G. L.↗