3,938 research outputs found
Reduced Order Modeling for Transonic Aeroservoelastic Control Law Development
As aircraft become more flexible, aeroelastic considerations become increasingly important and complex, particularly for transonic flight where nonlinearities in the flow render linear analysis tools less effective. In order to analyze these aeroelastic interactions between the fluid and the structure efficiently, reduced order models (ROMs) are sometimes generated from and used in place of computational fluid dynamics solutions. In this paper, several aerodynamic ROMs are generated and coupled with structural models to form aeroelastic ROMs. The aerodynamic ROMs generated here include the effects of control surface motion. Hence, the aeroelastic ROMs presented here are appropriate for use in aeroservoelastic applications and are intended to be used for aeroservoelastic control law development. These ROMs are used to simulate a number of test cases with and without control surface involvement. Results show that several of the ROMs generated in the paper are able to predict results similar to solutions of higher-order computational methods
Active Flutter Suppression Using Reduced-Order Modeling for Transonic Aeroservoelastic Control Law Development
In this paper, several aerodynamic reduced-order models (ROMs) are generated and coupled with structural models to form aeroelastic ROMs. The aerodynamic ROMs generated here include the effects of control surface motion and are appropriate for use in aeroservoelastic applications. Simple observer-based full-state feedback controllers were designed from these aeroelastic ROMs. Additionally, observer gain matrices were designed from and coupled to the aeroelastic ROMs. Each (linear) observer was then used to estimate the dynamics of a (nonlinear) stand-alone computational fluid-structure dynamics simulation. Then, using the estimated states and the full-state feedback controller, control surface commands were fed back into the computational fluid-structure dynamics simulation to successfully achieve active flutter suppression. The process, as well as some results, are presented in this paper
Winds of Planet Hosting Stars
The field of exoplanetary science is one of the most rapidly growing areas of
astrophysical research. As more planets are discovered around other stars, new
techniques have been developed that have allowed astronomers to begin to
characterise them. Two of the most important factors in understanding the
evolution of these planets, and potentially determining whether they are
habitable, are the behaviour of the winds of the host star and the way in which
they interact with the planet. The purpose of this project is to reconstruct
the magnetic fields of planet hosting stars from spectropolarimetric
observations, and to use these magnetic field maps to inform simulations of the
stellar winds in those systems using the Block Adaptive Tree Solar-wind Roe
Upwind Scheme (BATS-R-US) code. The BATS-R-US code was originally written to
investigate the behaviour of the Solar wind, and so has been altered to be used
in the context of other stellar systems. These simulations will give
information about the velocity, pressure and density of the wind outward from
the host star. They will also allow us to determine what influence the winds
will have on the space weather environment of the planet. This paper presents
the preliminary results of these simulations for the star Bo\"otis,
using a newly reconstructed magnetic field map based on previously published
observations. These simulations show interesting structures in the wind
velocity around the star, consistent with the complex topology of its magnetic
field.Comment: 8 pages, 2 figures, accepted for publication in the peer-reviewed
proceedings of the 14th Australian Space Research Conference, held at the
University of South Australia, 29th September - 1st October 201
Indication of Non-equilibrium Transport in SiGe p-MOSFETs
No abstract avaliable
A protosolar nebula origin for the ices agglomerated by Comet 67P/Churyumov-Gerasimenko
The nature of the icy material accreted by comets during their formation in
the outer regions of the protosolar nebula is a major open question in
planetary science. Some scenarios of comet formation predict that these bodies
agglomerated from crystalline ices condensed in the protosolar nebula.
Concurrently, alternative scenarios suggest that comets accreted amorphous ice
originating from the interstellar cloud or from the very distant regions of the
protosolar nebula. On the basis of existing laboratory and modeling data, we
find that the N/CO and Ar/CO ratios measured in the coma of the Jupiter
family comet 67P/Churyumov-Gerasimenko by the ROSINA instrument aboard the
European Space Agency's Rosetta spacecraft match those predicted for gases
trapped in clathrates. If these measurements are representative of the bulk
N/CO and Ar/CO ratios in 67P/Churyumov-Gerasimenko, it implies that the
ices accreted by the comet formed in the nebula and do not originate from the
interstellar medium, supporting the idea that the building blocks of outer
solar system bodies have been formed from clathrates and possibly from pure
crystalline ices. Moreover, because 67P/Churyumov-Gerasimenko is impoverished
in Ar and N, the volatile enrichments observed in Jupiter's atmosphere
cannot be explained solely via the accretion of building blocks with similar
compositions and require an additional delivery source. A potential source may
be the accretion of gas from the nebula that has been progressively enriched in
heavy elements due to photoevaporation.Comment: The Astrophysical Journal Letters, in pres
Natural Connections Demonstration Project, 2012- 2016: Final Report
This report presents the key findings from the Natural Connections Demonstration Project, that aimed to encourage teachers to take curricular learning outdoors. The project was commissioned by DEFRA, Natural England and Historic England, and delivered by a team at Plymouth University. 125 schools contributed to the evaluation which found that: 1. schools most likely to engage with outdoor learning displayed strong leadership and were open-minded about trying new things 2. schools reported a statistically-significant increase in the amount of time spent on outdoor learning activity across the project 3. Schools adopted many different models of outdoor learning 4. Schools invested time, goodwill, energy and funding in outdoor learning 5. Over 90 per cent of responding schools agreed that outdoor learning was useful for curriculum delivery 6. Outdoor learning had positive impacts for teachers and pupils 7. the project model of distributed independent brokerage was found to have the capacity to unlock latent demand for outdoor learning in schools, and to support schools in embedding low-cost outdoor learning practice
Chemical dynamics of triacetylene formation and implications to the synthesis of polyynes in Titan's atmosphere
For the last four decades, the role of polyynes such as diacetylene (HCCCCH) and triacetylene (HCCCCCCH) in the chemical evolution of the atmosphere of Saturn's moon Titan has been a subject of vigorous research. These polyacetylenes are thought to serve as an UV radiation shield in planetary environments; thus, acting as prebiotic ozone, and are considered as important constituents of the visible haze layers on Titan. However, the underlying chemical processes that initiate the formation and control the growth of polyynes have been the least understood to date. Here, we present a combined experimental, theoretical, and modeling study on the synthesis of the polyyne triacetylene (HCCCCCCH) via the bimolecular gas phase reaction of the ethynyl radical (CCH) with diacetylene (HCCCCH). This elementary reaction is rapid, has no entrance barrier, and yields the triacetylene molecule via indirect scattering dynamics through complex formation in a single collision event. Photochemical models of Titan's atmosphere imply that triacetylene may serve as a building block to synthesize even more complex polyynes such as tetraacetylene (HCCCCCCCCH)
Natural Connections Demonstration Project, 2012-2016: Analysis of the Key Evaluation Questions
This report provides a detailed discussion of the key evaluation questions relating to the impact of the Natural Connections Demonstration Project. The project's aim was to encourage teachers to take curricular learning outside
Doppler images and the underlying dynamo. The case of AF Leporis
The (Zeeman-)Doppler imaging studies of solar-type stars very often reveal
large high-latitude spots. This also includes F stars that possess relatively
shallow convection zones, indicating that the dynamo operating in these stars
differs from the solar dynamo. We aim to determine whether mean-field dynamo
models of late-F type dwarf stars can reproduce the surface features recovered
in Doppler maps. In particular, we wish to test whether the models can
reproduce the high-latitude spots observed on some F dwarfs. The photometric
inversions and the surface temperature maps of AF Lep were obtained using the
Occamian-approach inversion technique. Low signal-to-noise spectroscopic data
were improved by applying the least-squares deconvolution method. The locations
of strong magnetic flux in the stellar tachocline as well as the surface fields
obtained from mean-field dynamo solutions were compared with the observed
surface temperature maps. The photometric record of AF Lep reveals both long-
and short-term variability. However, the current data set is too short for
cycle-length estimates. From the photometry, we have determined the rotation
period of the star to be 0.9660+-0.0023 days. The surface temperature maps show
a dominant, but evolving, high-latitude (around +65 degrees) spot. Detailed
study of the photometry reveals that sometimes the spot coverage varies only
marginally over a long time, and at other times it varies rapidly. Of a suite
of dynamo models, the model with a radiative interior rotating as fast as the
convection zone at the equator delivered the highest compatibility with the
obtained Doppler images.Comment: accepted for publication in Astronomy & Astrophysic
DE 1 RIMS operational characteristics
The Retarding Ion Mass Spectrometer (RIMS) on the Dynamics Explorer 1 spacecraft observes both the thermal and superthermal (50 eV) ions of the ionosphere and inner magnetosphere. It is capable of measuring the detailed species distribution function of these ions in many cases. It was equipped with an integral electrometer to permit in-flight calibration of the detector sensitivities and variations thereof. A guide to understanding the RIMS data set is given. The reduction process from count rates to physical quantities is discussed in some detail. The procedure used to establish in-flight calibration is described, and results of a comparison with densities from plasma wave measurements are provided. Finally, a discussion is provided of various anomalies in the data set, including changes of channeltron efficiency with time, spin modulation of the axial sensor heads, apparent potential differences between the sensor heads, and failures of the radial head retarding potential sweep and of the -Z axial head aperture plane bias. Studies of the RIMS data set should be conducted only with a thorough awareness of the material presented here, or in collaboration with one of the scientists actively involved with RIMS data analysis
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