2,279 research outputs found
The Influence of Dust Formation Modelling on Na I and K I Line Profiles in Substellar Atmospheres
We aim to understand the correlation between cloud formation and alkali line
formation in substellar atmospheres.We perform line profile calculations for Na
I and K I based on the coupling of our kinetic model for the formation and
composition of dust grains with 1D radiative transfer calculations in
atmosphere models for brown dwarfs and giant gas planets. The Na I and K I line
profiles sensibly depend on the way clouds are treated in substellar atmosphere
simulations. The kinetic dust formation model results in the highest
pseudo-continuum compared to the limiting cases.Comment: 5 pages, Accepted for publication in MNRA
Entanglement and particle correlations of Fermi gases in harmonic traps
We investigate quantum correlations in the ground state of noninteracting
Fermi gases of N particles trapped by an external space-dependent harmonic
potential, in any dimension. For this purpose, we compute one-particle
correlations, particle fluctuations and bipartite entanglement entropies of
extended space regions, and study their large-N scaling behaviors. The
half-space von Neumann entanglement entropy is computed for any dimension,
obtaining S_HS = c_l N^(d-1)/d ln N, analogously to homogenous systems, with
c_l=1/6, 1/(6\sqrt{2}), 1/(6\sqrt{6}) in one, two and three dimensions
respectively. We show that the asymptotic large-N relation S_A\approx \pi^2
V_A/3, between the von Neumann entanglement entropy S_A and particle variance
V_A of an extended space region A, holds for any subsystem A and in any
dimension, analogously to homogeneous noninteracting Fermi gases.Comment: 15 pages, 22 fig
Complexity of links in 3-manifolds
We introduce a natural-valued complexity c(X) for pairs X=(M,L), where M is a
closed orientable 3-manifold and L is a link contained in M. The definition
employs simple spines, but for well-behaved X's we show that c(X) equals the
minimal number of tetrahedra in a triangulation of M containing L in its
1-skeleton. Slightly adapting Matveev's recent theory of roots for graphs, we
carefully analyze the behaviour of c under connected sum away from and along
the link. We show in particular that c is almost always additive, describing in
detail the circumstances under which it is not. To do so we introduce a certain
(0,2)-root for a pair X, we show that it is well-defined, and we prove that X
has the same complexity as its (0,2)-root. We then consider, for links in the
3-sphere, the relations of c with the crossing number and with the hyperbolic
volume of the exterior, establishing various upper and lower bounds. We also
specialize our analysis to certain infinite families of links, providing rather
accurate asymptotic estimates.Comment: 24 pages, 6 figure
Dust in brown dwarfs and extra-solar planets IV. Assessing TiO2 and SiO nucleation for cloud formation modeling
Clouds form in atmospheres of brown dwarfs and planets. The cloud particle
formation processes are similar to the dust formation process studied in
circumstellar shells of AGB stars and in Supernovae. Cloud formation modelling
in substellar objects requires gravitational settling and element replenishment
in addition to element depletion. All processes depend on the local conditions,
and a simultaneous treatment is required. We apply new material data in order
to assess our cloud formation model results regarding the treatment of the
formation of condensation seeds. We re-address the question of the primary
nucleation species in view of new (TiO2)_N-cluster data and new SiO vapour
pressure data. We apply the density functional theory using the computational
chemistry package Gaussian 09 to derive updated thermodynamical data for
(TiO2)_N-clusters as input for our TiO2 seed formation model. We test different
nucleation treatments and their effect on the overall cloud structure by
solving a system of dust moment equations and element conservation or a
pre-scribed Drift-Phoenix atmosphere structure. Updated Gibbs free energies for
the (TiO2)_N-clusters are presented, and a slightly temperature dependent
surface tension for T=500 ... 2000K with an average value of sigma_infty =
480.6 erg 1/cm2. The TiO2-seed formation rate changes only slightly with the
updated cluster data. A considerably larger effect on the rate of seed
formation, and hence on grain size and dust number density, results from a
switch to SiO-nucleation. Despite the higher abundance of SiO over TiO2 in the
gas phase, TiO2 remains considerably more efficient in forming condensation
seeds by homogeneous nucleation followed by heterogeneous grain growth. The
paper discussed the effect on the cloud structure in more detail.Comment: accepted for publication in A&A (abstract abridged
Structure Space of Model Proteins --A Principle Component Analysis
We study the space of all compact structures on a two-dimensional square
lattice of size . Each structure is mapped onto a vector in
-dimensions according to a hydrophobic model. Previous work has shown that
the designabilities of structures are closely related to the distribution of
the structure vectors in the -dimensional space, with highly designable
structures predominantly found in low density regions. We use principal
component analysis to probe and characterize the distribution of structure
vectors, and find a non-uniform density with a single peak. Interestingly, the
principal axes of this peak are almost aligned with Fourier eigenvectors, and
the corresponding Fourier eigenvalues go to zero continuously at the
wave-number for alternating patterns (). These observations provide a
stepping stone for an analytic description of the distribution of structural
points, and open the possibility of estimating designabilities of realistic
structures by simply Fourier transforming the hydrophobicities of the
corresponding sequences.Comment: 14 pages, 12 figures, Conclusion has been modifie
Polymer state approximations of Schroedinger wave functions
It is shown how states of a quantum mechanical particle in the Schroedinger
representation can be approximated by states in the so-called polymer
representation. The result may shed some light on the semiclassical limit of
loop quantum gravity.Comment: 11 pages, 1 figure, Conclusions section adde
Optical linear polarization in ultra cool dwarfs: A tool to probe dust in the ultra cool dwarf atmospheres
Aims.Recent studies have detected linear polarization in L dwarfs in the
optical I band. Theoretical models have been developed to explain this
polarization. These models predict higher polarization at shorter wavelengths.
We discuss the polarization in the R and I band of 4 ultra cool dwarfs.
Methods.We report linear polarization measurements of 4 ultra cool dwarfs in
the R and I bands using the Intermediate dispersion Spectrograph and Imaging
System (ISIS) mounted on the 4.2m William Herschel Telescope (WHT). Results.As
predicted by theoretical models, we find a higher degree of polarization in the
R band when compared to polarization in the I band for 3/4 of these ultra cool
dwarfs. This suggests that dust scattering asymmetry is caused by oblateness
>.We also show how these measurements fit the theoretical models. A case for
variability of linear polarization is found, which suggests the presence of
randomly distributed dust clouds. We also discuss one case for the presence of
a cold debris disk.Comment: 7 pages, 2 figure
Emission lines in the atmosphere of the irradiated brown dwarf WD0137−349B
ESL acknowledges the support of STFC studentship. SLC acknowledges support from the University of Leicester College of Science and Engineering. CH highlights the financial support of the European community under the FP7 ERC starting grant 257431. This work was supported by the Science and Technology Facilities Council [ST/M001040/1].We present new optical and near-infrared spectra of WD0137−349; a close white dwarf–brown dwarf non-interacting binary system with a period of ≈114 min. We have confirmed the presence of H α emission and discovered He, Na, Mg, Si, K, Ca, Ti and Fe emission lines originating from the brown-dwarf atmosphere. This is the first brown-dwarf atmosphere to have been observed to exhibit metal emission lines as a direct result of intense irradiation. The equivalent widths of many of these lines show a significant difference between the day-side and night-side of the brown dwarf. This is likely an indication that efficient heat redistribution may not be happening on this object, in agreement with models of hot Jupiter atmospheres. The H α line strength variation shows a strong phase dependency as does the width. We have simulated the Ca ii emission lines using a model that includes the brown-dwarf Roche geometry and limb darkening, and we estimate the mass ratio of the system to be 0.135 ± 0.004. We also apply a gas-phase equilibrium code using a prescribed drift-phoenix model to examine how the chemical composition of the brown-dwarf upper atmosphere would change given an outward temperature increase, and discuss the possibility that this would induce a chromosphere above the brown-dwarf atmosphere.Publisher PDFPeer reviewe
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