7,996 research outputs found
Alternate multiple-outer-planet missions using a Saturn-Jupiter flyby sequence
A study has been made of a method for providing more frequent launch opportunities for multiple-planet Grand Tour type missions to the outer solar system. A Saturn-Jupiter flyby sequence was used in the analysis to initiate the mission instead of the normal Jupiter-Saturn sequence. The Saturn-first approach is shown to yield several new launch opportunities following the 1980 cutoff date for Jupiter-first missions. Results are given for various two-planet, three-planet, and four-planet Jupiter-first and Saturn-first missions. A unique five-planet Saturn-first mission and a Saturn-Jupiter flyby which returns to earth are also discussed. Mission performance is evaluated for each flyby technique by comparing Saturn-first and Jupiter-first missions with respect to launch energy requirements, available launch windows, planetary encounter conditions, and total mission times
Flutter Investigation of 60 Degree to 80 Degree Delta-Planform Surfaces at a Mach Number of 7.0
The flutter characteristics of a series of half-span delta surfaces which had leading-edge sweep angles ranging from 60 degrees to 80 degrees were investigated in helium flaw at a Mach number of 7.0 in the Langley hypersonic aeroelasticity tunnel. For each value of sweep angle both wedge and double-wedge airfoil sections were tested at two pitch-axis positions, The models were mounted so that a rigid-body flapping-pitching type of flutter was encountered. Analysis of the results and comparison with theory show that the wedge models are more stable than the corresponding double-wedge models; the pitch-axis location at or near the center of gravity is more stable than the more forward location; the effects of leading-edge sweep angle on the flutter characteristics appear to be small; and an uncoupled-mode piston-theory analysis gave the best agreement with the experimental results
Legal Services: Meeting New Challenges with Delivery Systems that Promise Lasting Impact for Maryland\u27s Poor
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Spire stimulates nucleation by Cappuccino and binds both ends of actin filaments.
The actin nucleators Spire and Cappuccino synergize to promote actin assembly, but the mechanism of their synergy is controversial. Together these proteins promote the formation of actin meshes, which are conserved structures that regulate the establishment of oocyte polarity. Direct interaction between Spire and Cappuccino is required for oogenesis and for in vitro synergistic actin assembly. This synergy is proposed to be driven by elongation and the formation of a ternary complex at filament barbed ends, or by nucleation and interaction at filament pointed ends. To mimic the geometry of Spire and Cappuccino in vivo, we immobilized Spire on beads and added Cappuccino and actin. Barbed ends, protected by Cappuccino, grow away from the beads while pointed ends are retained, as expected for nucleation-driven synergy. We found that Spire is sufficient to bind barbed ends and retain pointed ends of actin filaments near beads and we identified Spire's barbed-end binding domain. Loss of barbed-end binding increases nucleation by Spire and synergy with Cappuccino in bulk pyrene assays and on beads. Importantly, genetic rescue by the loss-of-function mutant indicates that barbed-end binding is not necessary for oogenesis. Thus, increased nucleation is a critical element of synergy both in vitro and in vivo
Limits on Clouds and Hazes for the TRAPPIST-1 Planets
The TRAPPIST-1 planetary system is an excellent candidate for study of the
evolution and habitability of M-dwarf planets. Transmission spectroscopy
observations performed with the Hubble Space Telescope (HST) suggest the
innermost five planets do not possess clear hydrogen atmospheres. Here we
reassess these conclusions with recently updated mass constraints and expand
the analysis to include limits on metallicity, cloud top pressure, and the
strength of haze scattering. We connect recent laboratory results of particle
size and production rate for exoplanet hazes to a one-dimensional atmospheric
model for TRAPPIST-1 transmission spectra. Doing so, we obtain a
physically-based estimate of haze scattering cross sections. We find haze
scattering cross sections on the order of 1e-26 to 1e-19 cm squared are needed
in hydrogen-rich atmospheres for TRAPPIST-1 d, e, and f to match the HST data.
For TRAPPIST-1 g, we cannot rule out a clear hydrogen-rich atmosphere. We also
modeled the effects an opaque cloud deck and substantial heavy element content
have on the transmission spectra. We determine that hydrogen-rich atmospheres
with high altitude clouds, at pressures of 12mbar and lower, are consistent
with the HST observations for TRAPPIST-1 d and e. For TRAPPIST-1 f and g, we
cannot rule out clear hydrogen-rich cases to high confidence. We demonstrate
that metallicities of at least 60xsolar with tropospheric (0.1 bar) clouds
agree with observations. Additionally, we provide estimates of the precision
necessary for future observations to disentangle degeneracies in cloud top
pressure and metallicity. Our results suggest secondary, volatile-rich
atmospheres for the outer TRAPPIST-1 planets d, e, and f.Comment: 15 pages, 3 figures, 2 tables, accepted in the Astronomical Journa
Coronal response to an EUV wave from DEM analysis
EUV (Extreme-Ultraviolet) waves are globally propagating disturbances that
have been observed since the era of the SoHO/EIT instrument. Although the
kinematics of the wave front and secondary wave components have been widely
studied, there is not much known about the generation and plasma properties of
the wave. In this paper we discuss the effect of an EUV wave on the local
plasma as it passes through the corona. We studied the EUV wave, generated
during the 2011 February 15 X-class flare/CME event, using Differential
Emission Measure diagnostics. We analyzed regions on the path of the EUV wave
and investigated the local density and temperature changes. From our study we
have quantitatively confirmed previous results that during wave passage the
plasma visible in the Atmospheric Imaging Assembly (AIA) 171A channel is
getting heated to higher temperatures corresponding to AIA 193A and 211A
channels. We have calculated an increase of 6 - 9% in density and 5 - 6% in
temperature during the passage of the EUV wave. We have compared the variation
in temperature with the adiabatic relationship and have quantitatively
demonstrated the phenomenon of heating due to adiabatic compression at the wave
front. However, the cooling phase does not follow adiabatic relaxation but
shows slow decay indicating slow energy release being triggered by the wave
passage. We have also identified that heating is taking place at the front of
the wave pulse rather than at the rear. Our results provide support for the
case that the event under study here is a compressive fast-mode wave or a
shock.Comment: Accepted for publication in Ap
Hard X-ray footpoint sizes and positions as diagnostics of flare accelerated energetic electrons in the low solar atmosphere
The hard X-ray (HXR) emission in solar flares comes almost exclusively from a
very small part of the flaring region, the footpoints of magnetic loops. Using
RHESSI observations of solar flare footpoints, we determine the radial
positions and sizes of footpoints as a function of energy in six near-limb
events to investigate the transport of flare accelerated electrons and the
properties of the chromosphere. HXR visibility forward fitting allows to find
the positions/heights and the sizes of HXR footpoints along and perpendicular
to the magnetic field of the flaring loop at different energies in the HXR
range. We show that in half of the analyzed events, a clear trend of decreasing
height of the sources with energy is found. Assuming collisional thick-target
transport, HXR sources are located between 600 and 1200 km above the
photosphere for photon energies between 120 and 25 keV respectively. In the
other events, the position as a function of energy is constant within the
uncertainties. The vertical sizes (along the path of electron propagation)
range from 1.3 to 8 arcseconds which is up to a factor 4 larger than predicted
by the thick-target model even in events where the positions/heights of HXR
sources are consistent with the collisional thick-target model. Magnetic
mirroring, collisional pitch angle scattering and X-ray albedo are discussed as
potential explanations of the findings.Comment: 10 pages, 8 figures, accepted for publication in Ap
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An investigation into the psychometric properties of the CORE-OM in patients with eating disorders
Aim: The current study aimed to explore the psychometric properties of the CORE‐OM (Clinical Outcomes in Routine Evaluation – Outcome Measure) when used in an eating disorder sample. Method: The CORE‐OM was administered at assessment to 360 individuals referred to an eating disorders service. Principal component analysis was conducted to look at the psychometric structure of the CORE‐OM, and psychometric properties were investigated using analyses of reliability and validity. Results: Analyses of the psychometric structure suggested a three‐component solution reflecting negatively worded, positively worded and risk items. The CORE‐OM showed good acceptability, acceptable internal and test‐retest reliabilities, as well as good convergent and known groups validity. Conclusions: The results of the current study support the CORE‐OM as a reliable and valid measure for assessing psychological distress in eating disorders
Global implementation of Good Participatory Practice Guidelines for biomedical HIV prevention research: charting progress and setting milestones
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