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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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8 records
All sourcesNASA NTRSDOE OSTI
NASA NTRS1989

Heterodyne spectroscopy of the J = 17-16 CO line in Orion

High-resolution spectra of the 153 micron J = 17-16 CO line in the BN-KL region of Orion using a laser heterodyne spectrometer are obtained. The line shows broad wings characteristic of the plateau emission as well as a narrower component probably associated with the quiescent gas in the molecular ridge. From an analysis of the plateau emission together with that observed in lower J CO transitions, an excitation temperature of 180 + or - 50 K and minimum column density of 1 x 10 to the 18th /sq cm are derived for CO in this component, which constitutes 80 percent of the total integrated intensity of the J = 17-16 line near BN. The peak intensity of the narrower component observed at 0.8 km/s resolution increases relative to that of the plateau component toward theta 1C and away from BN, while the width decreases from 10 to 4 km/s (FWHM).

Boreiko, R. T.↗
NASA NTRS1989

Heterodyne spectroscopy of the J = 17-16 CO line in Orion

We have obtained high-resolution spectra of the 153 micrometers J = 17-16 CO line in the BN-KL region of Orion using a laser heterodyne spectrometer. The line shows broad wings (30 km s-1 FWHM at BN) characteristic of the plateau emission as well as a narrower component probably associated with the quiescent gas in the molecular ridge. From an analysis of the plateau emission together with that observed in lower J CO transitions, we derive an excitation temperature of 180 +/- 50 K and minimum column density of 1 x 10(18) cm-2 for CO in this component, which constitutes 80% of the total integrated intensity of the J = 17-16 line near BN. The peak intensity of the narrower component observed at 0.8 km s-1 resolution increases relative to that of the plateau component toward theta 1C and away from BN, while the width decreases from 10 to 4 km s-1 (FWHM).

NASA Discipline Number 52-60↗
DOE OSTI2018

Fallon FORGE: Lithology Logs and Well 21-31 Drilling Data

This submission includes lithology logs for all Fallon FORGE area wells; determined from core, cuttings, and thin section. Wells included are 84-31, 21-31, 82-36, FOH-3D, 62-36, 18-5, 88-24, 86-25, FOH-2, 14-36, 17-16, 34-33, 35A-11, 51A-20, 62-15, 72-7, 86-15, Carson_Strat_1_36-32, and several others. Lithology logs last updated 3/13/2018 with confirmation well 21-31 data, and revisited existing wells. Also included is well logging data for Fallon FORGE 21-31. Well logging data includes daily reports, well logs (drill rate, lithology, fractures, mud losses, minerals, temperature, gases, and descriptions), mud reports, drilling parameter plots, daily mud loss summaries, survey reports, progress reports, plan view maps (easting, northing), and wireline logs (caliper [with GR], triple combo [GR, caliper, SP, resistivity, array induction, density, photoelectric factor, and neutron porosity], array induction with linear correlation [GR, SP, Array Induction, caliper, conductivity], and monopole compression dipole shear [GR, SP, Caliper, sonic porosity, delta-T compressional, and delta-T shear])

15 GEOTHERMAL ENERGY↗
NASA NTRS1989

Heterodyne spectroscopy of the J = 22-21 CO line in Orion

The J = 22-21 line of (C-12)O at 2528 GHz was observed in the IRc2 region of Orion. The spectra at 0.6 km/s resolution show both plateau emission with FWHM of about 35 km/s and a narrower component with FWHM of about 8 km/s. Comparison with heterodyne data of similar quality on the J = 17-16 line indicates that the broad and narrow components both originate in gas with an excitation temperature of about 600 K.

Boreiko, R. T.↗
NASA NTRS1993

158 micron forbidden C II mapping of the Orion molecular cloud

A fully sampled, 1000-point, 1-arcmin-resolution map of the inner 6.5 x 10 arcmin (alpha x delta) regions of the Orion Nebula in the 157.7409-micron forbidden fine-structure line is constructed. Large-scale strip maps in forbidden C II across the face of the Orion molecular cloud, and CO(17-16), (14-13), and (7-6) spectra are obtained at selected positions in the Orion H II region/molecular cloud interface. Strong forbidden C II line emission is observed across the face of the Orion molecular. The total forbidden C II luminosity from the Orion molecular cloud is about 1500 solar luminosities, or 0.3 percent of the FIR luminosity. The extended forbidden C II emission probably arises in either the UV-exposed surface of the molecular cloud or from the surfaces of UV-exposed clumps within the molecular cloud.

Stacey, G. J.↗
NASA NTRS1994

Observations of High Rotational Excitation of CO Lines in AGB and Post-AGB Stars

We present ground based observations of AGB stars for CO J=6-5; 4-3; 3-2; 2-1 and 1-0 lines. Radiative transfer modelling of these lines suggests that the stars do not lose mass continuously, but undergo discrete bursts of significant mass loss. Ratio of brightness of different fines show a wide range of behaviours in different stars, with higher transition lines probing deeper into the circumstellar envelope. We also obtained higher CO rotational transitions for post-AGB stars at J=22-21; 17-16 and 13-12. These lines can be used as probes for the warm medium at the inner part of the envelope. From these results, we can trace the history of mass loss in these stars.

Justtanont, K.↗
NASA NTRS1989

Heterodyne spectroscopy of the J = 22-21 CO line in Orion

We have observed the J = 22-21 line of 12CO at 2528 GHz (118.8 micrometers) in the IRc2 region of Orion. The spectra at 0.6 km s-1 resolution show both plateau emission with FWHM approximately 35 km s-1 and a narrower component with FWHM approximately 8 km s-1. Comparison with heterodyne data of similar quality on the J = 17-16 line indicates that the broad and narrow components both originate in gas with an excitation temperature Tex approximately 600 K. The emission is consistent with the predictions of shock models in which the wide component arises from the heated outflow gas and postshock molecular material, while the narrow component comes from ambient material near the leading edge of the shock front where temperatures are high but significant acceleration has not yet occurred.

NASA Discipline Exobiology↗
DOE OSTI2016

Fallon FORGE: Well Data, Geophysical Data, and Geologic Maps

The data is associated to the Fallon FORGE project and includes mudlogs for all wells used to characterize the subsurface, as wells as gravity, magnetotelluric, earthquake seismicity, and temperature data from the Navy GPO and Ormat. Also included are geologic maps from the USGS and Nevada Bureau of Mines and Geology for the Fallon, NV area.

13-36↗