We then review a variety of sub jects: e.g., what ‘lives’ on I+ , the asymptotic Weyl tensor with the Bianchi Identities and the Bondi shear, other related structures as cuts of I+ , past-light-cones and angle ﬁelds.
On Extracting Physical Content from Asymptotically Flat Space-Time Metrics
Despite the absence of any signi ﬁcant shear, the mag netic ﬁelds realized in the simulations had structure on a broad range of spatial scales, and included a substantial large-scale component.
The rotation-magnetic field relation
Non-equilibrium properties, such as shear viscosity, bulk viscosity, thermal conductivity and neutrino emissivity, play an important role in constraining the structure of compact stars.
Phase Structure and Transport Properties of Dense Quark Matter
By contrast, values of qn may be chosen so that each eigenmode of the system with nontrivial radial structure (i.e. m > 0) may be stably inﬂuenced by the shear Q1 , yet, there is no such conﬁguration of the disturbed shear ﬂow that can act to stabilize a channel mode.
Low magnetic-Prandtl number flow configurations for cold astrophysical disk models: speculation and analysis
This proﬁle for Q has a top-hat structure and this descriptor will be used interchangeably with the expression symmetric shear step.
Low magnetic-Prandtl number flow configurations for cold astrophysical disk models: speculation and analysis
The main mode of instability and driver of turbulence in the numerical experiments of the shearing box is the channel mode which is a special response with no radial structure.
Low magnetic-Prandtl number flow configurations for cold astrophysical disk models: speculation and analysis
The direction eα changes slowly for typical light rays , whereas the dust shear is correlated with the shape and orientation of structures and changes on the length scale of those structures.
Backreaction in late-time cosmology
This excess power on small scales is expected, since structures within scales smaller than [sensor size]/n cannot be modeled by a polynomial of order n, where [sensor size]∼ 18(cid:48) in our simulations, the part of the PSF not modeled by the polynomial prints through as spurious shear correlation.
Spurious Shear in Weak Lensing with LSST
Since the cosmic shear described in this section directly probes the total matter content of the universe, i.e., without any reference to the relation between mass and luminosity, it provides an ideal tool to investigate the large-scale structure of the cosmological density ﬁeld.
Weak Gravitational Lensing
Consequently, structures near the observer are weighted more strongly than for magni ﬁcation or shear effects.
Weak Gravitational Lensing
Combining results from cosmic-shear measurements with the power spectrum of the cosmic density ﬂuctuations as measured from the CMB will allow a sensitive test of the gravitational instability picture for structure formation.
Weak Gravitational Lensing
The comparison between observed cosmic shear and theory will at least partly involve the increasingly detailed numerical simulations of cosmic structure evolution, from which predictions for lensing observations can directly be obtained.
Weak Gravitational Lensing
The ﬁrst clear detection of lensing by large-scale structures was actually revealed by cosmic shear (van Waerbeke et al. 2000).
Cosmic Magnification
The small c44 also suggests that MOF5 could collapse into a potentially useful structure under certain shear-stress.
Lattice Dynamics of Metal-Organic Frameworks (MOFs): Neutron Inelastic Scattering and First-Principles Calculations
After having shown that the MOF5 structure is stable with a very small shear modulus, we now discuss the lattice dynamics properties at the zone center and along high-symmetry directions in the Brillouin zone.
Lattice Dynamics of Metal-Organic Frameworks (MOFs): Neutron Inelastic Scattering and First-Principles Calculations
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