1,248 research outputs found
Primordial Earth mantle heterogeneity caused by the Moon-forming giant impact
The giant impact hypothesis for Moon formation successfully explains the
dynamic properties of the Earth-Moon system but remains challenged by the
similarity of isotopic fingerprints of the terrestrial and lunar mantles.
Moreover, recent geochemical evidence suggests that the Earth's mantle
preserves ancient (or "primordial") heterogeneity that predates the
Moon-forming giant impact. Using a new hydrodynamical method, we here show that
Moon-forming giant impacts lead to a stratified starting condition for the
evolution of the terrestrial mantle. The upper layer of the Earth is
compositionally similar to the disk, out of which the Moon evolves, whereas the
lower layer preserves proto-Earth characteristics. As long as this predicted
compositional stratification can at least partially be preserved over the
subsequent billions of years of Earth mantle convection, the compositional
similarity between the Moon and the accessible Earth's mantle is a natural
outcome of realistic and high-probability Moon-forming impact scenarios. The
preservation of primordial heterogeneity in the modern Earth not only
reconciles geochemical constraints but is also consistent with recent
geophysical observations. Furthermore, for significant preservation of a
proto-Earth reservoir, the bulk composition of the Earth-Moon system may be
systematically shifted towards chondritic values.Comment: Comments are welcom
Gremlin is a novel agonist of the major pro-angiogenic receptor VEGFR2
The bone morphogenic protein antagonist gremlin is expressed during embryonic development and under different pathologic conditions, including cancer. Gremlin is a proangiogenic protein belonging to the cystine-knot superfamily that includes transforming growth factor-β proteins and the angiogenic vascular endothelial growth factors (VEGFs). Here, we demonstrate that gremlin binds VEGF receptor-2 (VEGFR2), the main transducer of VEGF-mediated angiogenic signals, in a bone morphogenic protein-independent manner. Similar to VEGF-A, gremlin activates VEGFR2 in endothelial cells, leading to VEGFR2-dependent angiogenic responses in vitro and in vivo. Gremlin thus represents a novel proangiogenic VEGFR2 agonist distinct from the VEGF family ligands with implications in vascular development, angiogenesis-dependent diseases, and tumor neovascularization
Optimal strategies for gravitational wave stochastic background searches in pulsar timing data
A low frequency stochastic background of gravitational waves may be detected
by pulsar timing experiments in the next five to ten years. Using methods
developed to analyze interferometric gravitational wave data, in this paper we
lay out the optimal techniques to detect a background of gravitational waves
using a pulsar timing array. We show that for pulsar distances and
gravitational wave frequencies typical of pulsar timing experiments, neglecting
the effect of the metric perturbation at the pulsar does not result in a
significant deviation from optimality. We discuss methods for setting upper
limits using the optimal statistic, show how to construct skymaps using the
pulsar timing array, and consider several issues associated with realistic
analysis of pulsar timing data.Comment: 20 pages, 6 figures. Added figure with sky sensitivity for Parkes
Pulsar Timing Array, included dipole overlap reduction function and
derivation in appendix, extended likelihood discussio
Substrate-transferred GaAs/AlGaAs crystalline coatings for gravitational-wave detectors: A review of the state of the art
In this Perspective we summarize the status of technological development for
large-area and low-noise substrate-transferred GaAs/AlGaAs (AlGaAs) crystalline
coatings for interferometric gravitational-wave (GW) detectors. These topics
were originally presented in a workshop{\dag} bringing together members of the
GW community from the laser interferometer gravitational-wave observatory
(LIGO), Virgo, and KAGRA collaborations, along with scientists from the
precision optical metrology community, and industry partners with extensive
expertise in the manufacturing of said coatings. AlGaAs-based crystalline
coatings present the possibility of GW observatories having significantly
greater range than current systems employing ion-beam sputtered mirrors. Given
the low thermal noise of AlGaAs at room temperature, GW detectors could realize
these significant sensitivity gains, while potentially avoiding cryogenic
operation. However, the development of large-area AlGaAs coatings presents
unique challenges. Herein, we describe recent research and development efforts
relevant to crystalline coatings, covering characterization efforts on novel
noise processes, as well as optical metrology on large-area (~10 cm diameter)
mirrors. We further explore options to expand the maximum coating diameter to
20 cm and beyond, forging a path to produce low-noise AlGaAs mirrors amenable
to future GW detector upgrades, while noting the unique requirements and
prospective experimental testbeds for these novel materials.Comment: 13pages, 3 figure
Search for gravitational waves associated with the August 2006 timing glitch of the Vela pulsar
The physical mechanisms responsible for pulsar timing glitches are thought to excite quasinormal mode oscillations in their parent neutron star that couple to gravitational-wave emission. In August 2006, a timing glitch was observed in the radio emission of PSR B0833-45, the Vela pulsar. At the time of the glitch, the two colocated Hanford gravitational-wave detectors of the Laser Interferometer Gravitational wave observatory (LIGO) were operational and taking data as part of the fifth LIGO science run (S5). We present the first direct search for the gravitational-wave emission associated with oscillations of the fundamental quadrupole mode excited by a pulsar timing glitch. No gravitational-wave detection
candidate was found. We place Bayesian 90% confidence upper limits of 6.3 x 10^(-21) to 1.4 x 10^(-20) on the peak intrinsic strain amplitude of gravitational-wave ring-down signals, depending on which spherical harmonic mode is excited. The corresponding range of energy upper limits is 5.0 x 10^(-44) to 1.3 x 10^(-45) erg
Plume–ridge interactions: ridgeward versus plate-drag plume flow
The analysis of mid-ocean ridges and hotspots that are sourced by
deep-rooted mantle plumes allows us to get a glimpse of mantle structure and
dynamics. Dynamical interaction between ridge and plume processes have been
widely proposed and studied, particularly in terms of ridgeward plume flow.
However, the effects of plate drag on plume–lithosphere and plume–ridge
interaction remain poorly understood. In particular, the mechanisms that
control plume flow towards vs. away from the ridge have not yet been
systematically studied. Here, we use 2D thermomechanical numerical models of
plume–ridge interaction to systematically explore the effects of (i) ridge-spreading rate, (ii) initial plume head radius and (iii) plume–ridge
distance. Our numerical experiments suggest two different geodynamic
regimes: (1)Â plume flow towards the ridge is favored by strong buoyant
mantle plumes, slow spreading rates and small plume–ridge distances; (2) plume drag away from the ridge is in turn promoted by fast ridge spreading
for small-to-intermediate plumes and large plume–ridge distances. We find
that the pressure gradient between the buoyant plume and spreading ridge at
first drives ridgeward flow, but eventually the competition between plate
drag and the gravitational force of plume flow along the base of the sloping
lithosphere controls the fate of plume (spreading towards vs. away from the
ridge). Our results highlight that fast-spreading ridges exert strong plate-dragging force, which sheds new light on natural observations of largely
absent plume–lithosphere interaction along fast-spreading ridges, such as
the East Pacific Rise.</p
All-sky search for periodic gravitational waves in LIGO S4 data
We report on an all-sky search with the LIGO detectors for periodic
gravitational waves in the frequency range 50-1000 Hz and with the frequency's
time derivative in the range -1.0E-8 Hz/s to zero. Data from the fourth LIGO
science run (S4) have been used in this search. Three different semi-coherent
methods of transforming and summing strain power from Short Fourier Transforms
(SFTs) of the calibrated data have been used. The first, known as "StackSlide",
averages normalized power from each SFT. A "weighted Hough" scheme is also
developed and used, and which also allows for a multi-interferometer search.
The third method, known as "PowerFlux", is a variant of the StackSlide method
in which the power is weighted before summing. In both the weighted Hough and
PowerFlux methods, the weights are chosen according to the noise and detector
antenna-pattern to maximize the signal-to-noise ratio. The respective
advantages and disadvantages of these methods are discussed. Observing no
evidence of periodic gravitational radiation, we report upper limits; we
interpret these as limits on this radiation from isolated rotating neutron
stars. The best population-based upper limit with 95% confidence on the
gravitational-wave strain amplitude, found for simulated sources distributed
isotropically across the sky and with isotropically distributed spin-axes, is
4.28E-24 (near 140 Hz). Strict upper limits are also obtained for small patches
on the sky for best-case and worst-case inclinations of the spin axes.Comment: 39 pages, 41 figures An error was found in the computation of the C
parameter defined in equation 44 which led to its overestimate by 2^(1/4).
The correct values for the multi-interferometer, H1 and L1 analyses are 9.2,
9.7, and 9.3, respectively. Figure 32 has been updated accordingly. None of
the upper limits presented in the paper were affecte
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