235 research outputs found
Automatic normal orientation in point clouds of building interiors
Orienting surface normals correctly and consistently is a fundamental problem
in geometry processing. Applications such as visualization, feature detection,
and geometry reconstruction often rely on the availability of correctly
oriented normals. Many existing approaches for automatic orientation of normals
on meshes or point clouds make severe assumptions on the input data or the
topology of the underlying object which are not applicable to real-world
measurements of urban scenes. In contrast, our approach is specifically
tailored to the challenging case of unstructured indoor point cloud scans of
multi-story, multi-room buildings. We evaluate the correctness and speed of our
approach on multiple real-world point cloud datasets
Quantum Field Theoretic Description of Matter in the Universe
Quantum field theory at finite temperature and density can be used for
describing the physics of relativistic plasmas. Such systems are frequently
encountered in astrophysical situations, such as the early Universe, Supernova
explosions, and the interior of neutron stars. After a brief introduction to
thermal field theory the usefulness of this approach in astrophysics will be
exemplified in three different cases. First the interaction of neutrinos within
a Supernova plasma will be discussed. Then the possible presence of quark
matter in a neutron star core and finally the interaction of light with the
Cosmic Microwave Background will be considered.Comment: 7 pages, 9 figures, to be published in the Proceedings of the ISSI
Workshop "Matter in the Universe" (Bern, March 19-23, 2001), misprints
correcte
Quark phases in neutron stars and a "third family" of compact stars as a signature for phase transitions
The appearance of quark phases in the dense interior of neutron stars
provides one possibility to soften the equation of state (EOS) of neutron star
matter at high densities. This softening leads to more compact equilibrium
configurations of neutron stars compared to pure hadronic stars of the same
mass. We investigate the question to which amount the compactness of a neutron
star can be attributed to the presence of a quark phase. For this purpose we
employ several hadronic EOS in the framework of the relativistic mean-field
(RMF) model and an extended MIT bag model to describe the quark phase. We find
that - almost independent of the model parameters - the radius of a pure
hadronic neutron star gets typically reduced by 20-30% if a pure quark phase in
the center of the star does exist. For some EOS we furthermore find the
possibility of a "third family" of compact stars which may exist besides the
two known families of white dwarfs and neutron stars. We show how an
experimental proof of the existence of a third family by mass and radius
measurements may provide a unique signature for a phase transition inside
neutron stars.Comment: 37 pages, 18 eps-figures included, LaTe
Development of an antibody fragment that stabilizes GPCR/G-protein complexes.
Single-particle cryo-electron microscopy (cryo-EM) has recently enabled high-resolution structure determination of numerous biological macromolecular complexes. Despite this progress, the application of high-resolution cryo-EM to G protein coupled receptors (GPCRs) in complex with heterotrimeric G proteins remains challenging, owning to both the relative small size and the limited stability of these assemblies. Here we describe the development of antibody fragments that bind and stabilize GPCR-G protein complexes for the application of high-resolution cryo-EM. One antibody in particular, mAb16, stabilizes GPCR/G-protein complexes by recognizing an interface between Gα and Gβγ subunits in the heterotrimer, and confers resistance to GTPγS-triggered dissociation. The unique recognition mode of this antibody makes it possible to transfer its binding and stabilizing effect to other G-protein subtypes through minimal protein engineering. This antibody fragment is thus a broadly applicable tool for structural studies of GPCR/G-protein complexes
The influence of medium effects on the gross structure of hybrid stars
We investigate the influence of medium effects on the structure of hybrid
stars, i.e. neutron stars possessing a quark matter core. We found that medium
effects reduce the extent of a pure quark matter phase in the interior of a
hybrid star significantly in favor of a mixed phase of quark and hadronic
matter. Over a wide range of the strong coupling constant - which parameterizes
the influence of medium effects - quark matter is able to exist at least in a
mixed phase in the interior of neutron stars.Comment: 20 pages, LaTeX, 4 inline eps-figures, 4 gif-figures, extended
discussion, to be published in Nucl. Phys. A. Also available at
http://theorie.physik.uni-giessen.de/~schertle/HybSta
The hadron-quark phase transition in dense matter and neutron stars
We study the hadron-quark phase transition in the interior of neutron stars
(NS's). We calculate the equation of state (EOS) of hadronic matter using the
Brueckner-Bethe-Goldstone formalism with realistic two-body and three-body
forces, as well as a relativistic mean field model. For quark matter we employ
the MIT bag model constraining the bag constant by using the indications coming
from the recent experimental results obtained at the CERN SPS on the formation
of a quark-gluon plasma. We find necessary to introduce a density dependent bag
parameter, and the corresponding consistent thermodynamical formalism. We
calculate the structure of NS interiors with the EOS comprising both phases,
and we find that the NS maximum masses fall in a relatively narrow interval,
. The precise value of the
maximum mass turns out to be only weakly correlated with the value of the
energy density at the assumed transition point in nearly symmetric nuclear
matter.Comment: 25 pages, Revtex4, 16 figures included as postscrip
Complete relativistic equation of state for neutron stars
We construct the equation of state (EOS) in a wide density range for neutron
stars using the relativistic mean field theory. The properties of neutron star
matter with both uniform and non-uniform distributions are studied
consistently. The inclusion of hyperons considerably softens the EOS at high
densities. The Thomas-Fermi approximation is used to describe the non-uniform
matter, which is composed of a lattice of heavy nuclei. The phase transition
from uniform matter to non-uniform matter occurs around ,
and the free neutrons drip out of nuclei at about $2.4 \times 10^{-4}\
\rm{fm^{-3}}$. We apply the resulting EOS to investigate the neutron star
properties such as maximum mass and composition of neutron stars.Comment: 23 pages, REVTeX, 9 ps figures, to appear in Phys. Rev.
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