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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 181 records · Page 10
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NASA NTRS1985

Far-infrared observations of young clusters embedded in the R Coronae Australis and Rho Ophiuchi dark clouds

Multicolor far-infrared maps in two nearby dark clouds, R Coronae Australis and Rho Ophiuchi, have been made in order to investigate the individual contribution of low-mass stars to the energetics and dynamics of the surrounding gas and dust. Emission from cool dust associated with five low-mass stars has been detected in CrA and four in Rho Oph; their far-infrared luminosities range from 2 solar luminosities to 40 solar luminosities. When an estimate of the bolometric luminosity was possible, it was found that typically more than 50 percent of the star's energy was radiated longward of 20 microns. Meaningful limits to the far-infrared luminosities of an additional 11 association members in CrA and two in Rho Oph were also obtained. The dust optical depth surrounding the star R CrA appears to be asymmetric and may control the dynamics of the surrounding molecular gas. The implications of these results for the cloud energetics and star formation efficiency in these two clouds are discussed.

Wilking, B. A.↗
NASA NTRS1975

Far-infrared observations of W51 with high spatial resolution

Observations of the core of W51 have been made from the NASA C-141 Airborne Infrared Observatory at 55 microns with 17-, 35-, and 85-arc sec apertures and at 100 microns with a 35-arc sec aperture. These observations suggest the presence of a small less than about 20 arc sec source at 55 microns surrounded by a much broader diffuse background. In the center of the source the optical depth at 55 and 100 microns is on the order of 0.1-0.2.

Harvey, P. M.↗
NASA NTRS1976

Far infrared observations with a 1-m balloon-borne telescope

Properties of a balloon-borne inertially guided telescope designed to perform high-resolution mapping of far-IR sources are reviewed. Scientific results obtained to date are presented in terms of the sensitivity and angular resolution achieved. The objects observed and mapped include Orion A, W3, M43, OMC-2, NGC 7538, the infrared star IRC+10216, Uranus, and M82. Several modifications of the telescope are described which have markedly increased its IR sensitivity and its efficiency in acquiring sources.

Fazio, G. G.↗
NASA NTRS1976

Infrared observations of ices and silicates in molecular clouds

Spectrophotometric observations from 2 to 4 microns and from 8 to 13 microns of several infrared sources associated with molecular clouds are reported. Narrow absorption features at 3.08 microns, attributed to interstellar ices, appear in all sources with a molecular cloud in the intervening line of sight. All sources showing ice absorptions also show broad absorption features, attributed to cold silicates, from 8 to 13 microns. The observed ice absorption profiles are all quite similar; however, they do not fit in detail Mie theory predictions of extinction for pure H2O or NH3 ices. The ratio of ice-to-silicate optical depths is found to vary, with most sources showing a ratio in the range 0.1-0.4. The ratio of visual extinction to ice absorption is found to increase rapidly from inside to outside the molecular cloud in NGC 2024.

Merrill, K. M.↗
NASA NTRS1994

Relationship between ice water path and downward longwave radiation for clouds optically thin in the infrared: Observations and model calculations

A vertically pointing 3.2-cm radar is used to observe altostratus and cirrus clouds as they pass overhead. Radar reflectivities are used in combination with an empirical Z(sub i)-IWC (ice water content) relationship developed by Sassen (1987) to parameterize IWC, which is then integrated to obtain estimates of ice water path (IWP). The observed dataset is segregated into all-ice and mixed-phase periods using measurements of integrated liquid water paths (LWP) detected by a collocated, dual-channel microwave radiometer. The IWP values for the all ice periods are compared to measurements of infrared (IR) downward fluxes measured by a collocated narrowband (9.95-11.43 microns) IR radiometer, which results in scattergrams representing the observed dependence of IR fluxes on IWP. A two-stream model is used to calculate the infrared fluxes expected from ice clouds with boundary conditions specified by the actual clouds, and similar curves relating IWP and infrared fluxes are obtained. The model and observational results suggest that IWP is one of the primary controls on infrared thermal fluxes for ice clouds.

Uttal, Taneil↗
NASA NTRS2023

X-Ray and Near-Infrared Observations of the Middle-aged Pulsar B1055-52, Its Multiwavelength Spectrum, and Proper Motion

Previous observations of the middle-aged γ-ray, X-ray, and radio pulsar B1055–52 indicated some peculiarities, such as a suspected changing of the X-ray flux and spectral parameters, a large excess of the alleged thermal component of the UV spectrum over the Rayleigh–Jeans extension of the X-ray thermal spectrum, and a possible double break in the nonthermal spectral component between the optical and X-ray bands. We observed PSR B1055–52 with the XMM-Newton observatory in X-rays and the Hubble Space Telescope in near-infrared (NIR). The analysis of the XMM-Newton observations does not support the notion of long-term changes in the X-ray flux and broadband X-ray spectrum of the pulsar. Using an observing mode less affected by background noise than the previous XMM-Newton observations, we constrain the power-law (PL) spectral index as X 0.57 0.25 0.26 a = - - + (Fν ∝ ν α ) in the energy band 3–10 keV. From the NIR–optical data we obtain a PL slope αO = −0.24 ± 0.10 for the color index E(B − V ) = 0.03 mag. The slopes and fluxes of the NIR–optical and X-ray nonthermal spectra suggest that the NIR through X-ray emission can be described by the same PL and is generated by the same mechanism, unlike the pulsar’s γ-ray emission. The excess of the UV thermal component over the extension of the X-ray thermal component became smaller but did not disappear, indicating a nonuniformity of the bulk surface temperature. The NIR data also enable us to measure the proper motion accurately, with values μα = 47.5 ± 0.7 mas yr−1 and μδ = −8.7 ± 0.7 mas yr−1 .

B Posselt↗
NASA NTRS1989

Stratospheric H2(O-18) distribution from far infrared observations

The stratospheric distribution of H2(O-18) in the 22 to 37 km altitude range has been obtained from balloon-based measurement of far infrared thermal emission spectra with an unapodized spectral resolution of 0.0033/cm. The analysis is based on the observed spectra of 9 isolated spectral lines in the 46 to 72/cm region obtained from four complete limb sequences. Comparison of the results with the statistically expected values indicates enhancement in the H2(O-18) concentrations increasing from 27 + or - 14 percent at 29 km to 40 + or - 23 percent at 37 km. No significant enhancement at lower altitudes was observed.

Guo, J.↗
NASA NTRS1974

Infrared observations of comet Kohoutek near perihelion

Observations between 0.55 and 18 microns show that after perihelion passage, comet Kohoutek possessed an infrared tail and antitail. The coma and the tail have the silicate signature and contain 'black material' which acquires a temperature higher than the blackbody temperature at the given distance from the sun. The antitail shows the colors of a blackbody at a lower temperature, suggesting that the particles are larger than those in the coma and the tail.

Ney, E. P.↗
NASA NTRS1982

Visual and infrared observations of the distant Comets P/Stephan-Oterma /1980g/, Panther /1980u/, and Bowell /1980b/

The paper reports combined visual imagery and spectroscopy, near-infrared spectroscopy, and broadband infrared photometry of comets P/Stephan-Oterma (1980g), Bowell (1980b), and Panther (1980u) at intermediate heliocentric distances. The visual data indicate the existence of solid grains in extended halos around the nuclei of the three comets. Broadband near-infrared and thermal infrared measurements of Comet Panther suggest the presence of 2-4-micron-radius particles in the coma which most likely contain molecules incorporating the N-H bond, but which are more complex and less volatile than NH3. Such molecules can be produced in the grains by cosmic-ray reprocessing. Near infrared spectral features identical to those seen in comet Panther similary suggest the presence of a molecule incorporating the N-H bond in comet Bowell.

Jewitt, D. C.↗
NASA NTRS1972

Infrared observations of 1612 MHz IR/OH sources.

IR spectra and photometry are given for several IR objects which are known to have 1612 MHz OH emission. These IR/OH sources are shown to be either M type Mira variables or M supergiants with photospheric temperatures around 2000 K. All those examined are oxygen rich and none are carbon stars which suggests a high abundance of OH in their photospheres. A significant fraction of the total luminosity is emitted in the IR beyond 3.5 microns which is taken to imply a dust shell structure around the central star. There is no evidence which uniquely requires that IR pumping of the OH maser is taking place; there are, however, generally enough near infrared photons to supply the observed microwave energy.

Hyland, A. R.↗
NASA NTRS1988

Infrared observations of P/Halley and P/Encke

Broadband optical/infrared photometers responding from 0.5 to 23 microns mounted on the Univ. of Minnesota (UM) O'Brien 76-cm telescope, Wyoming Infrared Observatory 234-cm telescope, and UM's Mount Lemmon Infrared Observatory 152-cm telescope were used to measure comet Halley more than 30 times between 12 Dec. 1985 to 6 May 1986. The Wyoming system was used to measure P/Encke on 24 Jul. 1987. The equipment and observations of Halley were fully described by Gehrz and Ney. Conclusions based on a preliminary analysis of the Halley and P/Encke data are reported.

Gehrz, Robert D.↗
NASA NTRS1977

Far infrared observations of IRC + 10216

Results are reported for measurements of IRC + 10216 at 100 microns made with the 91-cm telescope of NASA's Kuiper Airborne Infrared Observatory. The IR photometer employed consisted of a gallium-doped germanium photoconductive detector with a MOSFET preamplifier and load resistor. Signals obtained from the source at modulation frequencies of 30 and 100 Hz are plotted, and the 100-micron flux measurements are shown to be in agreement with previous bolometric measurements. It is noted that the sensitivity of the photoconductive detection system is comparable to that of the conventional bolometers that have been used in airborne IR observations.

Shivanandan, K.↗
NASA NTRS1995

Infrared observations of an outburst of small dust grains from the nucleus of Comet P/Halley 1986 III at perihelion

A close examination of the 0.7- to 23-micron infrared data base acquired by Gehrz and Ney (1992), suggests that the nucleus of Comet P/Halley 1986 III emitted a burst of small dust grains during a 3-day period commencing within hours of perihelion passage on 1986 February 9.46 UT. The outburst was characterized by significant increases in the coma's grain color temperature T(sub obs), temperature excess (superheat: S = T(sub obs)/T(sub BB)), infrared luminosity, albedo, and 10-micron silicate emission feature strength. These changes are all consistent with the sudden ejection from the nucleus of a cloud of grains with radii of approximately 0.5 micron. This outburst may have produced the dust that was responsible for some of the tail streamers photographed on 1986 February 22 UT. The peak of the dust outburst occurred about 3 days before a pronounced increase in the water production rate measured by the Pioneer Venus Orbiter Ultraviolet Spectrometer. We suggest that jets that release large quantities of small particles may be largely responsible for some of the variable infrared behavior that has been reported for P/Halley and other comets during the past two decades. Such jets may also account for some of the differences IR Type I and IR Type II comets.

Gehrz, R. D.↗
NASA NTRS1993

Remote sensing cloud properties from high spectral resolution infrared observations

A technique for estimating cloud radiative properties (spectral emissivity and reflectivity) in the IR is developed based on observations at a spectral resolution of approximately 0.5/cm. The algorithm uses spectral radiance observations and theoretical calculations of the IR spectra for clear and cloudy conditions along with lidar-determined cloud-base and cloud-top pressure. An advantage of the high spectral resolution observations is that the absorption effects of atmospheric gases are minimized by analyzing between gaseous absorption lines. The technique is applicable to both ground-based and aircraft-based platforms and derives the effective particle size and associated cloud water content required to satisfy, theoretically, the observed cloud IR spectra. The algorithm is tested using theoretical simulations and applied to observations made with the University of Wisconsin's ground-based and NASA ER-2 aircraft High-Resolution Infrared Spectrometer instruments.

Smith, William L.↗
NASA NTRS1986

Simultaneous submillimeter and infrared observations of flat-spectrum radio sources

Observations are presented of 12 extragalactic nonthermal radio emission sources made at eight wavelengths between 1.25 and 1000 microns, including the important submillimeter wavelength of 350 microns. Nine of the objects were detected at 350 microns, roughly double the number of objects of this type that have previously been detected at this wavelength. The majority of the observations were made within a three-week time span. The results, combined with other studies, show that these objects generally have flat energy distributions at wavelengths longer than 1 mm that break in most cases between 350 microns and 1 mm. At wavelengths shorter than 1 mm, the energy distributions fall with a rough power-law behavior with a spectral index of about -1. For many of the objects, there is a definite break or curvature in the energy distributions at wavelengths near 2.2 microns, with the fluxes falling even more steeply into the near infrared. At the time of the observations, both OJ 287 and 3C 273 were undergoing flares. The results are generally consistent with the flares propagating out to longer wavelengths with time.

Roellig, T. L.↗