311 research outputs found
Gimballess Inertial Navigation Systems. Semi- Annual Progress Report, 1 Nov. 1964 - 30 Apr. 1965
Accelerometers for sensing angular velocity in gimballess inertial navigation syste
Modeling and Analysis of Power Processing Systems
The feasibility of formulating a methodology for the modeling and analysis of aerospace electrical power processing systems is investigated. It is shown that a digital computer may be used in an interactive mode for the design, modeling, analysis, and comparison of power processing systems
Thermodynamics of Element Volatility and its Application to Planetary Processes
Despite its importance in geological sciences, our understanding of
interactions between gas and condensed phases (comprising solids and liquids)
remains clouded by the fact that, often, only indirect evidence remains for
their occurrence. This arises from the tendency for the vapour phase to escape
from the condensed phase with which it interacts, owing to its much lower
density and thus greater volume. For a gas that is sufficiently tenuous that
interactions do not occur between its constituent molecules, this relationship
is quantified in the ideal gas law (Clapeyron 1834): (1) where is
the total pressure exerted by the gas, its volume, is the number of
moles, the gas constant 8.3145 , Horstmann, 1873) and
the absolute temperature. One mole of an ideal gas at 273.15 and
(standard temperature and pressure for gases) has a molar volume of 22,711
, x greater than typical silicate liquids or minerals. As a
result, vaporisation processes in nature are often informed by chemical and
textural evidence remaining in the condensed phase.Comment: 95 pages 19 figures 5 table
A review of the genus Empoasca (Homoptera: Cicadellidae) reported from northeast Kansas
Call number: LD2668 .T4 ENTM 1989 F44Master of ScienceEntomolog
The Deep Water Abundance on Jupiter: New Constraints from Thermochemical Kinetics and Diffusion Modeling
We have developed a one-dimensional thermochemical kinetics and diffusion
model for Jupiter's atmosphere that accurately describes the transition from
the thermochemical regime in the deep troposphere (where chemical equilibrium
is established) to the quenched regime in the upper troposphere (where chemical
equilibrium is disrupted). The model is used to calculate chemical abundances
of tropospheric constituents and to identify important chemical pathways for
CO-CH4 interconversion in hydrogen-dominated atmospheres. In particular, the
observed mole fraction and chemical behavior of CO is used to indirectly
constrain the Jovian water inventory. Our model can reproduce the observed
tropospheric CO abundance provided that the water mole fraction lies in the
range (0.25-6.0) x 10^-3 in Jupiter's deep troposphere, corresponding to an
enrichment of 0.3 to 7.3 times the protosolar abundance (assumed to be H2O/H2 =
9.61 x 10^-4). Our results suggest that Jupiter's oxygen enrichment is roughly
similar to that for carbon, nitrogen, and other heavy elements, and we conclude
that formation scenarios that require very large (>8 times solar) enrichments
in water can be ruled out. We also evaluate and refine the simple time-constant
arguments currently used to predict the quenched CO abundance on Jupiter, other
giant planets, and brown dwarfs.Comment: 42 pages, 7 figures, 4 tables, with note added in proof. Accepted for
publication in Icarus [in press
Atomic and Molecular Opacities for Brown Dwarf and Giant Planet Atmospheres
We present a comprehensive description of the theory and practice of opacity
calculations from the infrared to the ultraviolet needed to generate models of
the atmospheres of brown dwarfs and extrasolar giant planets. Methods for using
existing line lists and spectroscopic databases in disparate formats are
presented and plots of the resulting absorptive opacities versus wavelength for
the most important molecules and atoms at representative temperature/pressure
points are provided. Electronic, ro-vibrational, bound-free, bound-bound,
free-free, and collision-induced transitions and monochromatic opacities are
derived, discussed, and analyzed. The species addressed include the alkali
metals, iron, heavy metal oxides, metal hydrides, , , , ,
, , , and representative grains. [Abridged]Comment: 28 pages of text, plus 22 figures, accepted to the Astrophysical
Journal Supplement Series, replaced with more compact emulateapj versio
Elemental abundances and minimum mass of heavy elements in the envelope of HD 189733b
Oxygen (O) and carbon (C) have been inferred recently to be subsolar in
abundance from spectra of the atmosphere of the transiting hot Jupiter HD
189733b. Yet, the mass and radius of the planet coupled with structure models
indicate a strongly supersolar abundance of heavy elements in the interior of
this object. Here we explore the discrepancy between the large amount of heavy
elements suspected in the planet's interior and the paucity of volatiles
measured in its atmosphere. We describe the formation sequence of the icy
planetesimals formed beyond the snow line of the protoplanetary disk and
calculate the composition of ices ultimately accreted in the envelope of HD
189733b on its migration pathway. This allows us to reproduce the observed
volatile abundances by adjusting the mass of ices vaporized in the envelope.
The predicted elemental mixing ratios should be 0.15--0.3 times solar in the
envelope of HD 189733b if they are fitted to the recent O and C determinations.
However, our fit to the minimum mass of heavy elements predicted by internal
structure models gives elemental abundances that are 1.2--2.4 times oversolar
in the envelope of HD189733b. We propose that the most likely cause of this
discrepancy is irradiation from the central star leading to development of a
radiative zone in the planet's outer envelope which would induce gravitational
settling of elements. Hence, all strongly irradiated extrasolar planets should
present subsolar abundances of volatiles. We finally predict that the
abundances of nitrogen (N), sulfur (S) and phosphorus (P) are of , and relative to
H, respectively in the atmosphere of HD 189733b.Comment: Accepted for publication in Astronomy & Astrophysic
Spectroscopic Detection of Carbon Monoxide in Two Late-type T Dwarfs
M band spectra of two late-type T dwarfs, 2MASS J09373487+2931409, and Gliese
570D, confirm evidence from photometry that photospheric CO is present at
abundance levels far in excess of those predicted from chemical equilibrium.
These new and unambiguous detections of CO, together with an earlier
spectroscopic detection of CO in Gliese 229B and existing M band photometry of
a large selection of T dwarfs, suggest that vertical mixing in the photosphere
drives the CO abundance out of chemical equilibrium and is a common, and likely
universal feature of mid-to-late type T dwarfs. The M band spectra allow
determinations of the time scale of vertical mixing in the atmosphere of each
object, the first such measurements of this important parameter in late T
dwarfs. A detailed analysis of the spectral energy distribution of 2MASS
J09373487+2931409 results in the following values for metallicity, temperature,
surface gravity, and luminosity: [M/H]~-0.3, T_eff=925-975K, log g=5.20-5.47,
log L/L_sun=-5.308 +/- 0.027. The age is 3-10 Gyr and the mass is in the range
45-69 M_Jup.Comment: 36 pages incl. 12 figures and 3 tables, accepted by Ap
Challenges and strategies to facilitate formulation development of pediatric drug products: Safety qualification of excipients
A public workshop entitled âChallenges and strategies to facilitate formulation development of pediatric drug productsâ focused on current status and gaps as well as recommendations for risk-based strategies to support the development of pediatric age-appropriate drug products. Representatives from industry, academia, and regulatory agencies discussed the issues within plenary, panel, and case-study breakout sessions. By enabling practical and meaningful discussion between scientists representing the diversity of involved disciplines (formulators, nonclinical scientists, clinicians, and regulators) and geographies (eg, US, EU), the Excipients Safety workshop session was successful in providing specific and key recommendations for defining paths forward. Leveraging orthogonal sources of data (eg. food industry, agro science), collaborative data sharing, and increased awareness of the existing sources such as the Safety and Toxicity of Excipients for Paediatrics (STEP) database will be important to address the gap in excipients knowledge needed for risk assessment. The importance of defining risk-based approaches to safety assessments for excipients vital to pediatric formulations was emphasized, as was the need for meaningful stakeholder (eg, patient, caregiver) engagement
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