963 research outputs found
High-CO2 Cloud Radiative Forcing Feedback Over Both Land and Ocean in a Global Climate Model
A positive feedback on high-latitude winter marine climate change involving convective clouds has recently been proposed using simple models. This feedback could help explain data from equable climates, e.g., the Eocene, and might be relevant for future climate. Here this convective cloud feedback is shown to be active in an atmospheric GCM in modern configuration (CAM) at CO2 = 2240 ppm and in a coupled GCM in Eocene configuration (CCSM) at CO2 = 560 ppm. Changes in boundary conditions that increase surface temperature have a similar effect as increases in CO2 concentration. It is also found that the high-latitude winter cloud radiative forcing over land increases with increases in surface temperature due to either increased CO2 or changes in boundary conditions, which could represent an important part of the explanation for warm continental interior winter surface temperatures during equable climates. This is due to increased low-level layered clouds caused by increased relative humidity
Unification and the Hierarchy from AdS5
In AdS5, the coupling for bulk gauge bosons runs logarithmically, not as a
power law. For this reason, one can preserve perturbative unification of
couplings. Depending on the cutoff, this can occur at a high scale. We discuss
subtleties in the calculation and present a regularization scheme motivated by
the holographic correspondence. We find that generically, as in the standard
model, the couplings almost unify. For specific choices of the cutoff and
number of scalar multiplets, there is good agreement between the measured
couplings and the assumption of high scale unification.Comment: 5 pages, 2 figure
Post-impact faulting of the holfontein granophyre dike of the vredefort impact structure, south africa, inferred from remote sensing, geophysics, and geochemistry
Better characterization features borne from long-term crustal modification processes is essential for understanding the dynamics of large basin-forming impact structures on Earth. Within the deeply eroded 2.02 Ga Vredefort Impact Structure in South Africa, impact melt dikes are exposed at the surface. In this study, we utilized a combination of field, remote sensing, electrical resistivity, magnetic, petrographical, and geochemical techniques to characterize one such impact melt dike, namely, the Holfontein Granophyre Dike (HGD), along with the host granites. The HGD is split into two seemingly disconnected segments. Geophysical modeling of both segments sug-gests that the melt rock does not penetrate below the modern surface deeper than 5 m, which was confirmed by a later transecting construction trench. Even though the textures and clast content are different in two segments, the major element, trace element, and O isotope compositions of each segment are indistinguishable
Encoding a qubit into multilevel subspaces
We present a formalism for encoding the logical basis of a qubit into
subspaces of multiple physical levels. The need for this multilevel encoding
arises naturally in situations where the speed of quantum operations exceeds
the limits imposed by the addressability of individual energy levels of the
qubit physical system. A basic feature of the multilevel encoding formalism is
the logical equivalence of different physical states and correspondingly, of
different physical transformations. This logical equivalence is a source of a
significant flexibility in designing logical operations, while the multilevel
structure inherently accommodates fast and intense broadband controls thereby
facilitating faster quantum operations. Another important practical advantage
of multilevel encoding is the ability to maintain full quantum-computational
fidelity in the presence of mixing and decoherence within encoding subspaces.
The formalism is developed in detail for single-qubit operations and
generalized for multiple qubits. As an illustrative example, we perform a
simulation of closed-loop optimal control of single-qubit operations for a
model multilevel system, and subsequently apply these operations at finite
temperatures to investigate the effect of decoherence on operational fidelity.Comment: IOPart LaTeX, 2 figures, 31 pages; addition of a numerical simulatio
Strength and variability of the Oligocene Southern Ocean surface temperature gradient
Large Oligocene Antarctic ice sheets co-existed with warm proximal waters offshore Wilkes Land. Here we provide a broader Southern Ocean perspective to such warmth by reconstructing the strength and variability of the Oligocene Australian-Antarctic latitudinal sea surface temperature gradient. Our Oligocene TEX86-based sea surface temperature record from offshore southern Australia shows temperate (20–29 °C) conditions throughout, despite northward tectonic drift. A persistent sea surface temperature gradient (~5–10 °C) exists between Australia and Antarctica, which increases during glacial intervals. The sea surface temperature gradient increases from ~26 Ma, due to Antarctic-proximal cooling. Meanwhile, benthic foraminiferal oxygen isotope decline indicates ice loss/deep-sea warming. These contrasting patterns are difficult to explain by greenhouse gas forcing alone. Timing of the sea surface temperature cooling coincides with deepening of Drake Passage and matches results of ocean model experiments that demonstrate that Drake Passage opening cools Antarctic proximal waters. We conclude that Drake Passage deepening cooled Antarctic coasts which enhanced thermal isolation of Antarctica
Testing the Asteroseismic Mass Scale Using Metal-Poor Stars Characterized with APOGEE and Kepler
Fundamental stellar properties, such as mass, radius, and age, can be
inferred using asteroseismology. Cool stars with convective envelopes have
turbulent motions that can stochastically drive and damp pulsations. The
properties of the oscillation frequency power spectrum can be tied to mass and
radius through solar-scaled asteroseismic relations. Stellar properties derived
using these scaling relations need verification over a range of metallicities.
Because the age and mass of halo stars are well-constrained by astrophysical
priors, they provide an independent, empirical check on asteroseismic mass
estimates in the low-metallicity regime. We identify nine metal-poor red giants
(including six stars that are kinematically associated with the halo) from a
sample observed by both the Kepler space telescope and the Sloan Digital Sky
Survey-III APOGEE spectroscopic survey. We compare masses inferred using
asteroseismology to those expected for halo and thick-disk stars. Although our
sample is small, standard scaling relations, combined with asteroseismic
parameters from the APOKASC Catalog, produce masses that are systematically
higher (=0.17+/-0.05 Msun) than astrophysical expectations. The
magnitude of the mass discrepancy is reduced by known theoretical corrections
to the measured large frequency separation scaling relationship. Using
alternative methods for measuring asteroseismic parameters induces systematic
shifts at the 0.04 Msun level. We also compare published asteroseismic analyses
with scaling relationship masses to examine the impact of using the frequency
of maximum power as a constraint. Upcoming APOKASC observations will provide a
larger sample of ~100 metal-poor stars, important for detailed asteroseismic
characterization of Galactic stellar populations.Comment: 4 figures; 1 table. Accepted to ApJ
Kepler-432: a red giant interacting with one of its two long period giant planets
We report the discovery of Kepler-432b, a giant planet ()
transiting an evolved star with an orbital period of days. Radial velocities (RVs) reveal that
Kepler-432b orbits its parent star with an eccentricity of , which we also measure independently with
asterodensity profiling (AP; ), thereby confirming
the validity of AP on this particular evolved star. The well-determined
planetary properties and unusually large mass also make this planet an
important benchmark for theoretical models of super-Jupiter formation.
Long-term RV monitoring detected the presence of a non-transiting outer planet
(Kepler-432c; days), and adaptive optics imaging revealed a nearby
(0\farcs87), faint companion (Kepler-432B) that is a physically bound M dwarf.
The host star exhibits high signal-to-noise asteroseismic oscillations, which
enable precise measurements of the stellar mass, radius and age. Analysis of
the rotational splitting of the oscillation modes additionally reveals the
stellar spin axis to be nearly edge-on, which suggests that the stellar spin is
likely well-aligned with the orbit of the transiting planet. Despite its long
period, the obliquity of the 52.5-day orbit may have been shaped by star-planet
interaction in a manner similar to hot Jupiter systems, and we present
observational and theoretical evidence to support this scenario. Finally, as a
short-period outlier among giant planets orbiting giant stars, study of
Kepler-432b may help explain the distribution of massive planets orbiting giant
stars interior to 1 AU.Comment: 22 pages, 19 figures, 5 tables. Accepted to ApJ on Jan 24, 2015
(submitted Nov 11, 2014). Updated with minor changes to match published
versio
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