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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 145 records · Page 8
All sourcesNASA NTRSDOE OSTI
NASA NTRS2019

Risk Analysis Associated with Loss of Toxic Gases During Orion Landing and Recovery Operations

Mission, landing and recovery operations for the Orion crew module involve reentry into the Earth's atmosphere and the deployment of three Nomex parachutes to slow the descent before landing along the west coast of the United States. Orion may have residual fuel (hydrazine, N2H4) or coolant (ammonia, NH3) on board which are both highly toxic to crew in the event of exposure. These risks were evaluated using a first principles analysis approach through fluid dynamics modeling. Plume calculations were first performed with the ANSYS Fluent computational fluid dynamics code. Data were then extracted at locations relevant to crew safety such as the snorkel fan inlet and the egress hatch. Mixing calculations were performed to quantify exposure concentrations within the crew bay before and during egress and departure. Finally, results included herein were used to inform the Orion post-landing Concept of Operations (ConOps) so that strategies could be formulated to maintain crew safety in the event of the loss of fuel or coolant.

Orion↗
NASA NTRSDate not supplied

Orion Main Parachute Asymmetry Testing Revisited

Limited bridle-level asymmetry data were collected on three Orion main parachute cluster tests early in the development program. The results were published contemporaneously using analysis techniques developed by the Ares parachute program. Both programs seemed to indicate that large parachutes could develop line asymmetries far larger than what was assumed in design guides. Unfortunately, no additional asymmetry data were collected during Orion parachute development to corroborate these results. Recent high-fidelity data from Commercial Crew Program parachute system tests reinforce these legacy results. A method was developed to estimate suspension line-level asymmetry by “un-averaging” Orion bridle-level measurements using assumptions gleaned from the recent CCP experience. Efforts were made to improve the visualization of load asymmetry and its relationship with parachute geometric shape deformations.

parachutes↗
NASA NTRSDate not supplied

Orion SysML Model, Digital Twin, and Lessons Learned for Artemis I

In 2015 it was recognized by NASA’s Orion Chief Engineer that NASA’s design insight into the Orion subsystems for Artemis I were not sufficient to provide traditional engineering support to flight operations. To address these concerns and provide an opportunity to apply emerging model-based systems engineering and digital twin methodologies and provide opportunities for employees across NASA to get hands-on training, an Orion digital twin pilot project was initiated in 2020. With the increase in complexities of spacecraft, and decreased time to made decisions during missions in critical or emergency situations, digital modeling and integration of design can reduce the time to answer questions by days and required human resources by an order of magnitude over historical approaches and was identified to be critical capability for NASA’s future. This paper describes the genesis of this digital twin pilot project, efforts undertaken, a reproducible methodology to take available system information from a mature program to create an executable SysML model that supports a link to unit-specific data, thus forming a connection to the physical asset, and associated lessons learned and project deliverables.

MBSE↗
NASA NTRSDate not supplied

Analysis of the Artemis I Orion Spacecraft Power System Performance

NASA successfully completed an uncrewed test flight of the Orion spacecraft during the 26-day Artemis I mission in November and December 2022. The Artemis I mission profile included several potentially stressing features for Orion electrical power system (EPS) performance, including eclipse duration, multiple propulsive or navigational maneuvers which constrained positioning of the solar array wings (SAWs), and the proximity and phasing of various events together. All of these features vary significantly with Earth-sun-moon geometry, providing a unique challenge for predicting EPS performance before an exact launch date is known. This presentation will provide a brief mission overview, discuss the different computer models with varying levels of fidelity used to analyze Orion EPS performance, as well as the screening process developed to incorporate EPS performance as a consideration for launch epoch selection. Final preflight model predictions of EPS performance will be compared to in-flight telemetry measurements, and several EPS anomalies observed will be briefly discussed.

Orion↗
NASA NTRS2024

Design and Test of the Orion Crew Module Launch Abort System Hatch

The Orion spacecraft is part of NASA’s Artemis program to establish a permanent human presence on the lunar surface and further enable future crewed missions to Mars. One of the key safety features of Orion is the Launch Abort System (LAS) which pulls the Orion Crew Module (CM) away in the event of a launch vehicle malfunction. It was necessary to design a LAS hatch that allows for crew access to the CM during pad operations. This paper describes the background and evolution of the LAS hatch design, the features used to address the crew safety requirements, the testing challenges in preparation for the Artemis crewed missions, and lessons learned.

Hatch↗
NASA NTRSDate not supplied

Orion Artemis I Entry Performance

The Artemis I mission successfully demonstrated the Orion Multi-Purpose Crew Module ability to perform a skip re-entry with predictive guidance to reach the target splashdown location. Skip re-entry improves the down-range capability for precision landing, allowing Orion to return to the continental United States at any time during the lunar month, and improves the survivability from a wide range of return trajectories. This paper presents analysis of Orion skip re-entry Guidance and Control performance for the Artemis I mission utilizing recorded flight data and high fidelity simulation data. Descriptions of the related Guidance and Control designs are provided for understanding.

Artemis 1↗
NASA NTRSDate not supplied

Orion Artemis I Entry Performance

The Artemis I mission successfully demonstrated the Orion Multi-Purpose Crew Module ability to perform a skip re-entry with predictive guidance to reach the target splashdown location. Skip re-entry improves the down-range capability for precision landing, allowing Orion to return to the continental United States at any time during the lunar month, and improves the survivability from a wide range of return trajectories. This paper presents analysis of Orion skip re-entry Guidance and Control performance for the Artemis I mission utilizing recorded flight data and high fidelity simulation data. Descriptions of the related Guidance and Control designs are provided for understanding.

Artemis 1↗
NASA NTRS2024

Design and Test of the Orion Crew Module Launch Abort System Hatch

The Orion spacecraft is part of NASA’s Artemis program to establish a permanent human presence on the lunar surface and further enable future crewed missions to Mars. One of the key safety features of Orion is the Launch Abort System (LAS) which pulls the Orion Crew Module (CM) away in the event of a launch vehicle malfunction. It was necessary to design a LAS hatch that allows for crew access to the CM during pad operations. This paper describes the background and evolution of the LAS hatch design, the features used to address the crew safety requirements, the testing challenges in preparation for the Artemis crewed missions, and lessons learned.

Hatch↗
DOE OSTI2016

Three-dimensional shock structure of the Orion KL outflow with IGRINS

We report a study of the three-dimensional (3D) outflow structure of a 15″ × 13″ area around the H{sub 2} peak 1 in Orion KL with slit-scan observations (13 slits) using the Immersion Grating Infrared Spectrograph. The datacubes have a high-velocity resolution (∼7.5 km s{sup −1}), provide high-contrast imaging within ultra-narrow bands, and enable the detection of the main stream of the previously reported H{sub 2} outflow fingers. We identified 31 distinct fingers in the H{sub 2} 1−0 S(1) λ2.122 μm emission. The line profile at each finger shows multiple-velocity peaks with a strong low-velocity component around the systemic velocity at V{sub LSR} = +8 km s{sup −1} and high-velocity emission (|V{sub LSR}| = 45–135 km s{sup −1}), indicating a typical bow-shock. The observed radial velocity gradients of ∼4 km s{sup −1} arcsec{sup −1} agree well with the velocities inferred from large-scale proper motions, where the projected motion is proportional to the distance from a common origin. We construct a conceptual 3D map of the fingers with estimated inclination angles of 57°–74°. The extinction difference (ΔA {sub v} > 10 mag) between blueshifted and redshifted fingers indicates high internal extinction. The extinction, the overall angular spread, and the scale of the flow argue for an ambient medium with a very high density (10{sup 5}–10{sup 6} cm{sup −3}), consistent with molecular line observations of the Orion Molecular Cloud core. The radial velocity gradients and the 3D distributions of the fingers together support the hypothesis of a simultaneous radial explosion of the Orion KL outflow.

79 ASTRONOMY AND ASTROPHYSICS↗
DOE OSTI2017

Excitation of Molecular Hydrogen in the Orion Bar PhotodissociationRegion from a Deep Near-infrared IGRINS Spectrum

We present a deep near-infrared spectrum of the Orion Bar Photodissociation Region (PDR) taken with the Immersion Grating INfrared Spectrometer (IGRINS) on the 2.7 m telescope at the McDonald Observatory. IGRINS has high spectral resolution (R∼45,000) and instantaneous broad wavelength coverage (1.45–2.45 μm), enabling us to detect 87 emission lines from rovibrationally excited molecular hydrogen (H{sub 2}) that arise from transitions out of 69 upper rovibration levels of the electronic ground state. These levels cover a large range of rotational and vibrational quantum numbers and excitation energies, making them excellent probes of the excitation mechanisms of H{sub 2} and physical conditions within the PDR. The Orion Bar PDR is thought to consist of cooler high density clumps or filaments (T=50--250 K, n{sub H}=10{sup 5}--10{sup 7} cm{sup −3}) embedded in a warmer lower density medium (T=250--1000 K, n{sub H}=10{sup 4}--10{sup 5} cm{sup −3}). We fit a grid of constant temperature and density Cloudy models, which recreate the observed H{sub 2} level populations well, to constrain the temperature to a range of 600–650 K and the density to n{sub H}=2.5×10{sup 3}--10{sup 4} cm{sup −3}. The best-fit model gives T = 625 K and n{sub H}=5×10{sup 3} cm{sup −3}. This well-constrained warm temperature is consistent with kinetic temperatures found by other studies for the Orion Bar’s lower density medium. However, the range of densities well fit by the model grid is marginally lower than those reported by other studies. We could be observing lower density gas than the surrounding medium, or perhaps a density-sensitive parameter in our models is not properly estimated.

79 ASTRONOMY AND ASTROPHYSICS↗
DOE OSTI2017

The ALMA View of the OMC1 Explosion in Orion

Most massive stars form in dense clusters where gravitational interactions with other stars may be common. The two nearest forming massive stars, the BN object and Source I, located behind the Orion Nebula, were ejected with velocities of ∼29 and ∼13 km s{sup −1} about 500 years ago by such interactions. This event generated an explosion in the gas. New ALMA observations show in unprecedented detail, a roughly spherically symmetric distribution of over a hundred {sup 12}CO J = 2−1 streamers with velocities extending from V {sub LSR} = −150 to +145 km s{sup −1}. The streamer radial velocities increase (or decrease) linearly with projected distance from the explosion center, forming a “Hubble Flow” confined to within 50″ of the explosion center. They point toward the high proper-motion, shock-excited H{sub 2} and [Fe ii] “fingertips” and lower-velocity CO in the H{sub 2} wakes comprising Orion's “fingers.” In some directions, the H{sub 2} “fingers” extend more than a factor of two farther from the ejection center than the CO streamers. Such deviations from spherical symmetry may be caused by ejecta running into dense gas or the dynamics of the N -body interaction that ejected the stars and produced the explosion. This ∼10{sup 48} erg event may have been powered by the release of gravitational potential energy associated with the formation of a compact binary or a protostellar merger. Orion may be the prototype for a new class of stellar explosiozn responsible for luminous infrared transients in nearby galaxies.

79 ASTRONOMY AND ASTROPHYSICS↗
DOE OSTI2017

Which Stars Are Ionizing the Orion Nebula?

The common assumption that θ{sup 1} Ori C is the dominant ionizing source for the Orion Nebula is critically examined. This assumption underlies much of the existing analysis of the nebula. In this paper we establish through comparison of the relative strengths of emission lines with expectations from Cloudy models and through the direction of the bright edges of proplyds that θ{sup 2} Ori A, which lies beyond the Bright Bar, also plays an important role. θ{sup 1} Ori C does dominate ionization in the inner part of the Orion Nebula, but outside of the Bright Bar as far as the southeast boundary of the Extended Orion Nebula, θ{sup 2} Ori A is the dominant source. In addition to identifying the ionizing star in sample regions, we were able to locate those portions of the nebula in 3D. This analysis illustrates the power of MUSE spectral imaging observations to identify sources of ionization in extended regions.

79 ASTRONOMY AND ASTROPHYSICS↗
DOE OSTI2017

The Herschel Orion Protostar Survey: Luminosity and Envelope Evolution

The Herschel Orion Protostar Survey obtained well-sampled 1.2–870 μm spectral energy distributions (SEDs) of over 300 protostars in the Orion molecular clouds, home to most of the young stellar objects (YSOs) in the nearest 500 pc. We plot the bolometric luminosities and temperatures for 330 Orion YSOs, 315 of which have bolometric temperatures characteristic of protostars. The histogram of the bolometric temperature is roughly flat; 29% of the protostars are in Class 0. The median luminosity decreases by a factor of four with increasing bolometric temperature; consequently, the Class 0 protostars are systematically brighter than the Class I protostars, with a median luminosity of 2.3 L{sub ⊙} as opposed to 0.87 L{sub ⊙}. At a given bolometric temperature, the scatter in luminosities is three orders of magnitude. Using fits to the SEDs, we analyze how the luminosities corrected for inclination and foreground reddening relate to the mass in the inner 2500 au of the best-fit model envelopes. The histogram of the envelope mass is roughly flat, while the median-corrected luminosity peaks at 15 L{sub ⊙} for young envelopes and falls to 1.7 L{sub ⊙} for late-stage protostars with remnant envelopes. The spread in luminosity at each envelope mass is three orders of magnitude. Envelope masses that decline exponentially with time explain the flat mass histogram and the decrease in luminosity, while the formation of a range of stellar masses explains the dispersion in luminosity.

79 ASTRONOMY AND ASTROPHYSICS↗
NASA NTRS1974

Submillimeter observations of the Orion Nebula and NGC 2024

New observations at submillimeter wavelengths of the Orion Nebula and NGC 2024 are shown to provide a rather detailed map of the Orion Nebula at these wavelengths. The Orion Nebula emission is attributed to optically thin thermal radiation from dust grains in the molecular cloud with peak emission centered in the Kleinmann-Low nebula source.

Soifer, B. T.↗
NASA NTRS1978

Ultraviolet photometry from the orbiting astronomical observatory. XXX - The Orion reflection nebulosity

Surface-brightness measurements are presented that cover the region of Orion in nine intermediate-width bandpasses ranging from 4250 to 1550 A. The existence of an extended ultraviolet reflection nebulosity in this area is confirmed, and the characteristics of its spectrum and spatial distribution are derived. The observations are consistent with a model in which the dense molecular cloud complex in Orion is illuminated by the foreground Orion aggregate of early-type stars. The interpretation is complicated by the fact that foreground dust may contribute to the observed scattered light. The scattering particles in the cloud appear to exhibit a wavelength-dependent albedo similar to that found for interstellar grains in general, with a strong indication that the phase function changes to a less forward-scattering form in the ultraviolet.

Witt, A. N.↗
NASA NTRS1979

Two new methanol transitions in Orion A

Emission from the 11(1) - 10(2) (A-) and 5(0) - 4(1) (E) transitions of CH3OH at rest frequencies of 76,247.4 and 76,509.9 MHz, respectively, has been detected toward Orion A. The velocity widths of the two transitions are estimated to be approximately 3 km/s, which is consistent with other methanol lines in Orion. It is noted that the 117.5-kayser upper-state energy of the 11(1) - 10(2) (A-) transition is the highest yet reported for methanol in any source. The observed intensity is shown to be consistent with the 90-K thermal excitation model that seems to be appropriate for all other reported CH3OH lines in Orion A. Total column densities of 3 x 10 to the 16th per sq cm for the 11(1) - 10(2) (A-) transition and of 2 x 10 to the 16th per sq cm for the 5(0) - 4(1) (E) transition are calculated.

Jennings, D. E.↗
NASA NTRS1979

Measurements of the extinction to the molecular hydrogen emission from the Orion Nebula

Observations of the reddening of two pairs of H2 emission lines in the Orion Nebula are presented. A reddening of 0.8 + or - 0.2 mag between 2.12 and 2.42 microns is derived from observations of the intensity ratio of the v = 1-0 S(1) (2.12-micron) line and the Q(3) (2.42-micron) line and a comparison of this ratio with its unreddened value. The result is checked by a measurement of the intensity ratio of the v = 1-0 S(2) (2.03-micron) line and the Q(4) (2.43-micron) line. The total IR and visual extinctions to the emission region are inferred to be 4 + or - 1 mag (2.1 microns) and 40 + or - 10 mag (visual). Previous measurements of the H2 emission lines in Orion are corrected on the basis of these results, yielding a total H2 luminosity of approximately 2000 suns, an average column density of about 3 x 10 to the 20th per sq cm, and essentially equal rotational and vibrational temperatures (2000 K) for the H2. It is concluded that the H2 emission region in Orion lies within the molecular cloud, probably at the same depth as the IR cluster.

Beckwith, S.↗
NASA NTRS1983

The kinetic temperature and CH3CCH column density profiles in SGR B2, Orion, and Dr 21

Kinetic temperatures, T(kin), are presently estimated by means of a technique employing the intensities of the adjacent rotational transitions of symmetric top molecules, under the assumptions that the metastable levels are thermalized, and that the excitation temperature connecting the upper level of the observed transition to the lowest level in the K ladder is the same for the both adjacent transitions. The method is applied to observations of the J = 5-4 and J = 6-5 transitions of CH3CCH obtained at 1-arcmin intervals along a NS-EW cross that centered on Orion KL, Sgr B2, and Dr 21. The technique's application to CH3CN lines from the central positions of Sgr B2 and Orion produces T(kin) values that are in good agreement with other determinations. The fact that these lines are broader than those of CH3CCH is interpreted in terms of a model in which CH3CN emission is confined to small and warm core region while CH3CCH emission is dominated by a more extensive, almost isothermal and cooler halo region in Orion KL and Sgr B2.

Churchwell, E.↗