1,704 research outputs found
Comparative aeronomy of the upper atmosphere of the giant planets.
This thesis presents a study of H3 emission from Jupiter, Saturn and Uranus. This emission is associated with both auroral and solar processes, and can be used to trace energy inputs in the upper atmosphere. For Jupiter, a detailed analysis of the H3 emission is performed using a ID self-consistent atmospheric numerical model and the detailed balance formulation for H3 contained within a volume of H2. It is shown that the effects due to departures from local thermodynamic equilibrium (LTE) are significant, reducing the intensity of the observed H3. Evidence of this is shown to be present in published observations of the jovian aurora. Using the non-LTE results, the auroral heating event observed by Stallard et al. 2002 on Jupiter is analysed in terms of energy inputs and outputs. It is shown that the dominant heating source is Joule heating and ion-drag, produced by the increase in ion velocity in the auroral electrojet. However, in the absence of the heating there are not enough heat sinks as to cool down the atmosphere quickly, indicative that the energy is re-distributed mechanically via thermally driven winds. Using data from the United Kingdom Infrared Telescope (UKIRT), the first reliable auroral H3" temperature of Saturn is determined: T = 400 50 Kelvin with a column- integrated H3" density of N = 4.6 x 1016 m-2. The variations in column density within the dataset are large, indicating large variations in the precipitation flux, while the temperature remains fairly constant. On Uranus, infrared H3 spectra covering a decade is analysed in an attempt to explain the observed variability. This forms the most comprehensive long-term study of H3 emission to date. The variability is found to be complicated, with an auroral component of the total Hjj" emission being of similar magnitude as the EUV-produced component. The auroral component appears to be controlled by geometry
Cassini observations of ion and electron beams at Saturn and their relationship to infrared auroral arcs
We present Cassini Visual and Infrared Mapping Spectrometer observations of infrared auroral emissions from the noon sector of Saturn's ionosphere revealing multiple intense auroral arcs separated by dark regions poleward of the main oval. The arcs are interpreted as the ionospheric signatures of bursts of reconnection occurring at the dayside magnetopause. The auroral arcs were associated with upward field-aligned currents, the magnetic signatures of which were detected by Cassini at high planetary latitudes. Magnetic field and particle observations in the adjacent downward current regions showed upward bursts of 100–360 keV light ions in addition to energetic (hundreds of keV) electrons, which may have been scattered from upward accelerated beams carrying the downward currents. Broadband, upward propagating whistler waves were detected simultaneously with the ion beams. The acceleration of the light ions from low altitudes is attributed to wave-particle interactions in the downward current regions. Energetic (600 keV) oxygen ions were also detected, suggesting the presence of ambient oxygen at altitudes within the acceleration region. These simultaneous in situ and remote observations reveal the highly energetic magnetospheric dynamics driving some of Saturn's unusual auroral features. This is the first in situ identification of transient reconnection events at regions magnetically conjugate to Saturn's magnetopause
Exploring cosmic origins with CORE : Cluster science
We examine the cosmological constraints that can be achieved with a galaxy cluster survey with the future CORE space mission. Using realistic simulations of the millimeter sky, produced with the latest version of the Planck Sky Model, we characterize the CORE cluster catalogues as a function of the main mission performance parameters. We pay particular attention to telescope size, key to improved angular resolution, and discuss the comparison and the complementarity of CORE with ambitious future ground-based CMB experiments that could be deployed in the next decade. A possible CORE mission concept with a 150 cm diameter primary mirror can detect of the order of 50,000 clusters through the thermal Sunyaev-Zeldovich effect (SZE). The total yield increases (decreases) by 25% when increasing (decreasing) the mirror diameter by 30 cm. The 150 cm telescope configuration will detect the most massive clusters (> 10(14) M-circle dot) at redshift z > 1.5 over the whole sky, although the exact number above this redshift is tied to the uncertain evolution of the cluster SZE flux-mass relation; assuming self-similar evolution, CORE will detect similar to 500 clusters at redshift z > 1.5. This changes to 800 (200) when increasing (decreasing) the mirror size by 30 cm. CORE will be able to measure individual cluster halo masses through lensing of the cosmic microwave background anisotropies with a 1-sigma sensitivity of 4 x 10(14)M(circle dot), for a 120 cm aperture telescope, and 10(14)M(circle dot) for a 180 cm one. From the ground, we estimate that, for example, a survey with about 150,000 detectors at the focus of 350 cm telescopes observing 65% of the sky would be shallower than CORE and detect about 11,000 clusters, while a survey with the same number of detectors observing 25% of sky with a 10 m telescope is expected to be deeper and to detect about 70,000 clusters. When combined with the latter, CORE would reach a limiting mass of M-500 similar to 2-3 x 10(13)M(circle dot) and detect 220,000 clusters (5 sigma detection limit). Cosmological constraints from CORE cluster counts alone are competitive with other scheduled large scale structure surveys in the 2020's for measuring the dark energy equation of-state parameters w(0) and w(a) (sigma(w0) = 0.28, sigma(wa) = 0.31). In combination with primary CMB constraints, CORE cluster counts can further reduce these error bars on w(0) and w(a) to 0.05 and 0.13 respectively, and constrain the sum of the neutrino masses, Sigma m(nu), to 39 meV (1 sigma). The wide frequency coverage of CORE, 60-600 GHz, will enable measurement of the relativistic thermal SZE by stacking clusters. Contamination by dust emission from the clusters, however, makes constraining the temperature of the intracluster medium difficult. The kinetic SZE pairwise momentum will be extracted with S/N = 70 in the foreground cleaned CMB map. Measurements of T-CMB (z) using CORE clusters will establish competitive constraints on the evolution of the CMB temperature: (1 + z)(1-beta), with an uncertainty of sigma(beta) less than or similar to 2.7 x 10(-3) at low redshift (z less than or similar to 1). The wide frequency coverage also enables clean extraction of a map of the diffuse SZE signal over the sky, substantially reducing contamination by foregrounds compared to the Planck SZE map extraction. Our analysis of the one-dimensional distribution of Compton-y values in the simulated map finds an order of magnitude improvement in constraints on sigma(8) over the Planck result, demonstrating the potential of this cosmological probe with CORE.Peer reviewe
Prospects for high-z cluster detections with Planck, based on a follow-up of 28 candidates using MegaCam@CFHT
The Planck catalogue of SZ sources limits itself to a significance threshold
of 4.5 to ensure a low contamination rate by false cluster candidates. This
means that only the most massive clusters at redshift z>0.5, and in particular
z>0.7, are expected to enter into the catalogue, with a large number of systems
in that redshift regime being expected around and just below that threshold. In
this paper, we follow-up a sample of SZ sources from the Planck SZ catalogues
from 2013 and 2015. In the latter maps, we consider detections around and at
lower significance than the threshold adopted by the Planck Collaboration. To
keep the contamination rate low, our 28 candidates are chosen to have
significant WISE detections, in combination with non-detections in SDSS/DSS,
which effectively selects galaxy cluster candidates at redshifts .
By taking r- and z-band imaging with MegaCam@CFHT, we bridge the 4000A
rest-frame break over a significant redshift range, thus allowing accurate
redshift estimates of red-sequence cluster galaxies up to z~0.8. After
discussing the possibility that an overdensity of galaxies coincides -by
chance- with a Planck SZ detection, we confirm that 16 of the candidates have
likely optical counterparts to their SZ signals, 13 (6) of which have an
estimated redshift z>0.5 (z>0.7). The richnesses of these systems are generally
lower than expected given the halo masses estimated from the Planck maps.
However, when we follow a simplistic model to correct for Eddington bias in the
SZ halo mass proxy, the richnesses are consistent with a reference
mass-richness relation established for clusters detected at higher
significance. This illustrates the benefit of an optical follow-up, not only to
obtain redshift estimates, but also to provide an independent mass proxy that
is not based on the same data the clusters are detected with, and thus not
subject to Eddington bias.Comment: 13 pages, 7 figures. Accepted for publication in A&
The Origin of the Designability of Protein Structures
We examined what determines the designability of 2-letter codes (H and P)
lattice proteins from three points of view. First, whether the native structure
is searched within all possible structures or within maximally compact
structures. Second, whether the structure of the used lattice is bipartite or
not. Third, the effect of the length of the chain, namely, the number of
monomers on the chain. We found that the bipartiteness of the lattice structure
is not a main factor which determines the designability. Our results suggest
that highly designable structures will be found when the length of the chain is
sufficiently long to make the hydrophobic core consisting of enough number of
monomers.Comment: 17 pages, 2 figure
Identification of Berezin-Toeplitz deformation quantization
We give a complete identification of the deformation quantization which was
obtained from the Berezin-Toeplitz quantization on an arbitrary compact Kaehler
manifold. The deformation quantization with the opposite star-product proves to
be a differential deformation quantization with separation of variables whose
classifying form is explicitly calculated. Its characteristic class (which
classifies star-products up to equivalence) is obtained. The proof is based on
the microlocal description of the Szegoe kernel of a strictly pseudoconvex
domain given by Boutet de Monvel and Sjoestrand.Comment: 26 page
Force Distribution in a Granular Medium
We report on systematic measurements of the distribution of normal forces
exerted by granular material under uniaxial compression onto the interior
surfaces of a confining vessel. Our experiments on three-dimensional, random
packings of monodisperse glass beads show that this distribution is nearly
uniform for forces below the mean force and decays exponentially for forces
greater than the mean. The shape of the distribution and the value of the
exponential decay constant are unaffected by changes in the system preparation
history or in the boundary conditions. An empirical functional form for the
distribution is proposed that provides an excellent fit over the whole force
range measured and is also consistent with recent computer simulation data.Comment: 6 pages. For more information, see http://mrsec.uchicago.edu/granula
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