158 research outputs found
Protein folding mediated by solvation: water expelling and formation of the hydrophobic core occurs after the structure collapse
The interplay between structure-search of the native structure and
desolvation in protein folding has been explored using a minimalist model.
These results support a folding mechanism where most of the structural
formation of the protein is achieved before water is expelled from the
hydrophobic core. This view integrates water expulsion effects into the funnel
energy landscape theory of protein folding. Comparisons to experimental results
are shown for the SH3 protein. After the folding transition, a near-native
intermediate with partially solvated hydrophobic core is found. This transition
is followed by a final step that cooperatively squeezes out water molecules
from the partially hydrated protein core.Comment: Proceedings of the National Academy of Science, 2002, Vol.99. 685-69
Transit and Eclipse Analyses of Exoplanet HD 149026b Using BLISS Mapping
The dayside of HD 149026b is near the edge of detectability by the Spitzer
Space Telescope. We report on eleven secondary-eclipse events at 3.6, 4.5, 3 x
5.8, 4 x 8.0, and 2 x 16 microns plus three primary-transit events at 8.0
microns. The eclipse depths from jointly-fit models at each wavelength are
0.040 +/- 0.003% at 3.6 microns, 0.034 +/- 0.006% at 4.5 microns, 0.044 +/-
0.010% at 5.8 microns, 0.052 +/- 0.006% at 8.0 microns, and 0.085 +/- 0.032% at
16 microns. Multiple observations at the longer wavelengths improved
eclipse-depth signal-to-noise ratios by up to a factor of two and improved
estimates of the planet-to-star radius ratio (Rp/Rs = 0.0518 +/- 0.0006). We
also identify no significant deviations from a circular orbit and, using this
model, report an improved period of 2.8758916 +/- 0.0000014 days.
Chemical-equilibrium models find no indication of a temperature inversion in
the dayside atmosphere of HD 149026b. Our best-fit model favors large amounts
of CO and CO2, moderate heat redistribution (f=0.5), and a strongly enhanced
metallicity. These analyses use BiLinearly-Interpolated Subpixel Sensitivity
(BLISS) mapping, a new technique to model two position-dependent systematics
(intrapixel variability and pixelation) by mapping the pixel surface at high
resolution. BLISS mapping outperforms previous methods in both speed and
goodness of fit. We also present an orthogonalization technique for
linearly-correlated parameters that accelerates the convergence of Markov
chains that employ the Metropolis random walk sampler. The electronic
supplement contains light-curve files and supplementary figures.Comment: Accepted for publication in Ap
Protein structures and optimal folding emerging from a geometrical variational principle
Novel numerical techniques, validated by an analysis of barnase and
chymotrypsin inhibitor, are used to elucidate the paramount role played by the
geometry of the protein backbone in steering the folding to the correct native
state. It is found that, irrespective of the sequence, the native state of a
protein has exceedingly large number of conformations with a given amount of
structural overlap compared to other compact artificial backbones; moreover the
conformational entropies of unrelated proteins of the same length are nearly
equal at any given stage of folding. These results are suggestive of an
extremality principle underlying protein evolution, which, in turn, is shown to
be associated with the emergence of secondary structures.Comment: Revtex, 5 pages, 5 postscript figure
Infrared Eclipses of the Strongly Irradiated Planet WASP-33b, and Oscillations of its Host Star
We observe two secondary eclipses of the strongly irradiated transiting
planet WASP-33b in the Ks band, and one secondary eclipse each at 3.6- and 4.5
microns using Warm Spitzer. This planet orbits an A5V delta-Scuti star that is
known to exhibit low amplitude non-radial p-mode oscillations at about
0.1-percent semi-amplitude. We detect stellar oscillations in all of our
infrared eclipse data, and also in one night of observations at J-band out of
eclipse. The oscillation amplitude, in all infrared bands except Ks, is about
the same as in the optical. However, the stellar oscillations in Ks band have
about twice the amplitude as seen in the optical, possibly because the
Brackett-gamma line falls in this bandpass. We use our best-fit values for the
eclipse depth, as well as the 0.9 micron eclipse observed by Smith et al., to
explore possible states of the exoplanetary atmosphere, based on the method of
Madhusudhan and Seager. On this basis we find two possible states for the
atmospheric structure of WASP-33b. One possibility is a non-inverted
temperature structure in spite of the strong irradiance, but this model
requires an enhanced carbon abundance (C/O>1). The alternative model has solar
composition, but an inverted temperature structure. Spectroscopy of the planet
at secondary eclipse, using a spectral resolution that can resolve the water
vapor band structure, should be able to break the degeneracy between these very
different possible states of the exoplanetary atmosphere. However, both of
those model atmospheres absorb nearly all of the stellar irradiance with
minimal longitudinal re-distribution of energy, strengthening the hypothesis of
Cowan et al. that the most strongly irradiated planets circulate energy poorly.
Our measurement of the central phase of the eclipse yields e*cos(omega)=0.0003
+/-0.00013, which we regard as being consistent with a circular orbit.Comment: 23 pages, 9 figures, 3 tables, accepted for the Astrophysical Journa
The TRAPPIST survey of southern transiting planets. I. Thirty eclipses of the ultra-short period planet WASP-43 b
We present twenty-three transit light curves and seven occultation light
curves for the ultra-short period planet WASP-43 b, in addition to eight new
measurements of the radial velocity of the star. Thanks to this extensive data
set, we improve significantly the parameters of the system. Notably, the
largely improved precision on the stellar density (2.41+-0.08 rho_sun) combined
with constraining the age to be younger than a Hubble time allows us to break
the degeneracy of the stellar solution mentioned in the discovery paper. The
resulting stellar mass and size are 0.717+-0.025 M_sun and 0.667+-0.011 R_sun.
Our deduced physical parameters for the planet are 2.034+-0.052 M_jup and
1.036+-0.019 R_jup. Taking into account its level of irradiation, the high
density of the planet favors an old age and a massive core. Our deduced orbital
eccentricity, 0.0035(-0.0025,+0.0060), is consistent with a fully circularized
orbit. We detect the emission of the planet at 2.09 microns at better than
11-sigma, the deduced occultation depth being 1560+-140 ppm. Our detection of
the occultation at 1.19 microns is marginal (790+-320 ppm) and more
observations are needed to confirm it. We place a 3-sigma upper limit of 850
ppm on the depth of the occultation at ~0.9 microns. Together, these results
strongly favor a poor redistribution of the heat to the night-side of the
planet, and marginally favor a model with no day-side temperature inversion.Comment: 14 pages, 6 tables, 11 figures. Accepted for publication in A&
Spitzer observations of the thermal emission from WASP-43b
WASP-43b is one of the closest-orbiting hot Jupiters, with a semimajor axis
of a = 0.01526 +/- 0.00018 AU and a period of only 0.81 days. However, it
orbits one of the coolest stars with a hot Jupiter (Tstar = 4520 +/- 120 K),
giving the planet a modest equilibrium temperature of Teq = 1440 +/- 40 K,
assuming zero Bond albedo and uniform planetary energy redistribution. The
eclipse depths and brightness temperatures from our jointly fit model are
0.347% +/- 0.013% and 1670 +/- 23 K at 3.6 {\mu}m and 0.382% +/- 0.015% and
1514 +/- 25 K at 4.5 {\mu}m. The eclipse timings improved the estimate of the
orbital period, P, by a factor of three (P = 0.81347436 +/- 1.4*10-7 days) and
put an upper limit on the eccentricity (e = 0.010+0.010 -0.007). We use our
Spitzer eclipse depths along with four previously reported ground-based
photometric observations in the near-infrared to constrain the atmospheric
properties of WASP-43b. The data rule out a strong thermal inversion in the
dayside atmosphere of WASP-43b. Model atmospheres with no thermal inversions
and fiducial oxygen-rich compositions are able to explain all the available
data. However, a wide range of metallicities and C/O ratios can explain the
data. The data suggest low day-night energy redistribution in the planet,
consistent with previous studies, with a nominal upper limit of about 35% for
the fraction of energy incident on the dayside that is redistributed to the
nightside.Comment: 11 pages, 9 figure
Possible thermochemical disequilibrium in the atmosphere of the exoplanet GJ 436b
The nearby extrasolar planet GJ 436b--which has been labelled as a 'hot
Neptune'--reveals itself by the dimming of light as it crosses in front of and
behind its parent star as seen from Earth. Respectively known as the primary
transit and secondary eclipse, the former constrains the planet's radius and
mass, and the latter constrains the planet's temperature and, with measurements
at multiple wavelengths, its atmospheric composition. Previous work using
transmission spectroscopy failed to detect the 1.4-\mu m water vapour band,
leaving the planet's atmospheric composition poorly constrained. Here we report
the detection of planetary thermal emission from the dayside of GJ 436b at
multiple infrared wavelengths during the secondary eclipse. The best-fit
compositional models contain a high CO abundance and a substantial methane
(CH4) deficiency relative to thermochemical equilibrium models for the
predicted hydrogen-dominated atmosphere. Moreover, we report the presence of
some H2O and traces of CO2. Because CH4 is expected to be the dominant
carbon-bearing species, disequilibrium processes such as vertical mixing and
polymerization of methane into substances such as ethylene may be required to
explain the hot Neptune's small CH4-to-CO ratio, which is at least 10^5 times
smaller than predicted
Mean-Field HP Model, Designability and Alpha-Helices in Protein Structures
Analysis of the geometric properties of a mean-field HP model on a square
lattice for protein structure shows that structures with large number of switch
backs between surface and core sites are chosen favorably by peptides as unique
ground states. Global comparison of model (binary) peptide sequences with
concatenated (binary) protein sequences listed in the Protein Data Bank and the
Dali Domain Dictionary indicates that the highest correlation occurs between
model peptides choosing the favored structures and those portions of protein
sequences containing alpha-helices.Comment: 4 pages, 2 figure
Energy Landscape and Global Optimization for a Frustrated Model Protein
The three-color (BLN) 69-residue model protein was designed to exhibit frustrated folding. We investigate the energy landscape of this protein using disconnectivity graphs and compare it to a Go model, which is designed to reduce the frustration by removing all non-native attractive interactions. Finding the global minimum on a frustrated energy landscape is a good test of global optimization techniques, and we present calculations evaluating the performance of basin-hopping and genetic algorithms for this system.Comparisons are made with the widely studied 46-residue BLN protein.We show that the energy landscape of the 69-residue BLN protein contains several deep funnels, each of which corresponds to a different β-barrel structure
Suppressed Far-UV stellar activity and low planetary mass-loss in the WASP-18 system
WASP-18 hosts a massive, very close-in Jupiter-like planet. Despite its young age (R′HK activity parameter lies slightly below the basal level; there is no significant time-variability in the log R′HK value; there is no detection of the star in the X-rays. We present results of far-UV observations of WASP-18 obtained with COS on board of HST aimed at explaining this anomaly. From the star’s spectral energy distribution, we infer the extinction (E(B − V) ≈ 0.01mag) and then the ISM column density for a number of ions, concluding that ISM absorption is not the origin of the anomaly. We measure the flux of the four stellar emission features detected in the COS spectrum (C II, C III, C IV, Si IV). Comparing the C II/C IV flux ratio measured for WASP-18 with that derived from spectra of nearby stars with known age, we see that the far-UV spectrum of WASP-18 resembles that of old (>5Gyr), inactive stars, in stark contrast with its young age. We conclude that WASP-18 has an intrinsically low activity level, possibly caused by star-planet tidal interaction, as suggested by previous studies. Re-scaling the solar irradiance reference spectrum to match the flux of the Si IV line, yields an XUV integrated flux at the planet orbit of 10.2 erg s−1 cm−2. We employ the rescaled XUV solar fluxes to model of the planetary upper atmosphere, deriving an extremely low thermal mass-loss rate of 10−20MJ Gyr−1. For such high-mass planets, thermal escape is not energy limited, but driven by Jeans escape
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