69 research outputs found
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Advanced Cast Austenitic Stainless Steels for High Temperature Components
In July of 2002, a Cooperative Research and Development Agreement (CRADA) was undertaken between Oak Ridge National Laboratory (ORNL) and Caterpillar, Inc. (Caterpillar Technical Center) to develop and commercialize new cast stainless steels invented and initially tested on a prior CRADA. This CRADA is a direct follow-on project to CRADA ORNL-99-0533 for diesel engine exhaust component and gas turbine engine structural component applications. The goal of this new CRADA was to develop and commercialize the newly discovered cast stainless steels (primarily CF8C-Plus) with improved performance and reliability, as lower-cost upgrade alternatives to more costly cast Ni-based superalloys
Relationship between Intelligence and Criterion Task Set Performance1
↵1 This research was sponsored in part by the Workload and Ergonomics Branch of the Armstrong Aerospace Medical Research Laboratory, United States Air Force, under Contract F33615-85-D-0514 through the Southeastern Center for Electrical Engineering Education (SCEEEHER/86-9). The United States Government is authorized to reproduce and distribute reprints for government purposes notwithstanding any copyright notation hereon. The authors wish to thank Gary Reid for his interest and support in the completion of this projectYeshttps://us.sagepub.com/en-us/nam/manuscript-submission-guideline
CSO and CARMA Observations of L1157. I. A Deep Search for Hydroxylamine (NHOH)
A deep search for the potential glycine precursor hydroxylamine (NHOH)
using the Caltech Submillimeter Observatory (CSO) at mm and the
Combined Array for Research in Millimeter-wave Astronomy (CARMA) at mm is presented toward the molecular outflow L1157, targeting the B1 and B2
shocked regions. We report non-detections of NHOH in both sources. We a
perform non-LTE analysis of CHOH observed in our CSO spectra to derive
kinetic temperatures and densities in the shocked regions. Using these
parameters, we derive upper limit column densities of NHOH of ~cm and ~cm toward the B1
and B2 shocks, respectively, and upper limit relative abundances of
and ,
respectively.Comment: Accepted in the Astrophysical Journa
CSO and CARMA Observations of L1157. II. Chemical Complexity in the Shocked Outflow
L1157, a molecular dark cloud with an embedded Class 0 protostar possessing a
bipolar outflow, is an excellent source for studying shock chemistry, including
grain-surface chemistry prior to shocks, and post-shock, gas-phase processing.
The L1157-B1 and B2 positions experienced shocks at an estimated ~2000 and 4000
years ago, respectively. Prior to these shock events, temperatures were too low
for most complex organic molecules to undergo thermal desorption. Thus, the
shocks should have liberated these molecules from the ice grain-surfaces en
masse, evidenced by prior observations of SiO and multiple grain mantle species
commonly associated with shocks. Grain species, such as OCS, CH3OH, and HNCO,
all peak at different positions relative to species that are preferably formed
in higher velocity shocks or repeatedly-shocked material, such as SiO and HCN.
Here, we present high spatial resolution (~3") maps of CH3OH, HNCO, HCN, and
HCO+ in the southern portion of the outflow containing B1 and B2, as observed
with CARMA. The HNCO maps are the first interferometric observations of this
species in L1157. The maps show distinct differences in the chemistry within
the various shocked regions in L1157B. This is further supported through
constraints of the molecular abundances using the non-LTE code RADEX (Van der
Tak et al. 2007). We find the east/west chemical differentiation in C2 may be
explained by the contrast of the shock's interaction with either cold, pristine
material or warm, previously-shocked gas, as seen in enhanced HCN abundances.
In addition, the enhancement of the HNCO abundance toward the the older shock,
B2, suggests the importance of high-temperature O-chemistry in shocked regions.Comment: Accepted for publication in the Astrophysical Journa
Efficient production of S8 in interstellar ices: the effects of cosmic-ray-driven radiation chemistry and nondiffusive bulk reactions
Theoretical Chemistr
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Tensile and Creep-Rupture Evaluation of a New Heat of Haynes Alloy 25
From 1999 to 2006, a program was undertaken within the Materials Science and Technology Division, formerly the Metals and Ceramics Division, of Oak Ridge National Laboratory to characterize the tensile and creep-rupture properties of a newly produced heat of Haynes alloy 25 (L-605). Tensile properties from room temperature to 1100 C were evaluated for base material and welded joints aged up to 12,000 hours at 675 C. Creep and creep-rupture tests were conducted on base metal and cross-weldments from 650 to 950 C. Pressurized tubular creep tests were conducted to evaluate multiaxial creep-rupture response of the material. Over 800,000 hours of creep test data were generated during the test program with the longest rupture tests extending beyond 38,000 hours, and the longest creep-rate experiments exceeding 40,000 hours
A Search for Light Hydrides in the Envelopes of Evolved Stars
We report a search for the diatomic hydrides SiH, PH, and FeH along the line
of sight toward the chemically rich circumstellar envelopes of IRC+10216 and VY
Canis Majoris. These molecules are thought to form in high temperature regions
near the photospheres of these stars, and may then further react via gas-phase
and dust-grain interactions leading to more complex species, but have yet to be
constrained by observation. We used the GREAT spectrometer on SOFIA to search
for rotational emission lines of these molecules in four spectral windows
ranging from 600 GHz to 1500 GHz. Though none of the targeted species were
detected in our search, we report their upper limit abundances in each source
and discuss how they influence the current understanding of hydride chemistry
in dense circumstellar media. We attribute the non-detections of these hydrides
to their compact source sizes, high barriers of formation, and proclivity to
react with other molecules in the winds.Comment: Accepted for publication in ApJ. 14 pages, 4 figures, 3 table
Non-detection of HC_(11)N towards TMC-1: constraining the chemistry of large carbon-chain molecules
Bell et al. reported the first detection of the cyanopolyyne HC_(11)N towards the cold dark cloud TMC-1; no subsequent detections have been reported towards any source. Additional observations of cyanopolyynes and other carbon-chain molecules towards TMC-1 have shown a log-linear trend between molecule size and column density, and in an effort to further explore the underlying chemical processes driving this trend, we have analysed Green Bank Telescope observations of HC_9N and HC_(11)N towards TMC-1. Although we find an HC_9N column density consistent with previous values, HC_(11)N is not detected and we derive an upper limit column density significantly below that reported in Bell et al. Using a state-of-the-art chemical model, we have investigated possible explanations of non-linearity in the column density trend. Despite updating the chemical model to better account for ion–dipole interactions, we are not able to explain the non-detection of HC_(11)N, and we interpret this as evidence of previously unknown carbon-chain chemistry. We propose that cyclization reactions may be responsible for the depleted HC11N abundance, and that products of these cyclization reactions should be investigated as candidate interstellar molecules
Non-detection of HC_(11)N towards TMC-1: constraining the chemistry of large carbon-chain molecules
Bell et al. reported the first detection of the cyanopolyyne HC_(11)N towards the cold dark cloud TMC-1; no subsequent detections have been reported towards any source. Additional observations of cyanopolyynes and other carbon-chain molecules towards TMC-1 have shown a log-linear trend between molecule size and column density, and in an effort to further explore the underlying chemical processes driving this trend, we have analysed Green Bank Telescope observations of HC_9N and HC_(11)N towards TMC-1. Although we find an HC_9N column density consistent with previous values, HC_(11)N is not detected and we derive an upper limit column density significantly below that reported in Bell et al. Using a state-of-the-art chemical model, we have investigated possible explanations of non-linearity in the column density trend. Despite updating the chemical model to better account for ion–dipole interactions, we are not able to explain the non-detection of HC_(11)N, and we interpret this as evidence of previously unknown carbon-chain chemistry. We propose that cyclization reactions may be responsible for the depleted HC11N abundance, and that products of these cyclization reactions should be investigated as candidate interstellar molecules
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