12,368 research outputs found
Reservoir simulation and near-well bore modelling to aid scale management in a low temperature development with multilateral wells
A Search for Small-Scale Clumpiness in Dense Cores of Molecular Clouds
We have analyzed HCN(1-0) and CS(2-1) line profiles obtained with high
signal-to-noise ratios toward distinct positions in three selected objects in
order to search for small-scale structure in molecular cloud cores associated
with regions of high-mass star formation. In some cases, ripples were detected
in the line profiles, which could be due to the presence of a large number of
unresolved small clumps in the telescope beam. The number of clumps for regions
with linear scales of ~0.2-0.5 pc is determined using an analytical model and
detailed calculations for a clumpy cloud model; this number varies in the
range: ~2 10^4-3 10^5, depending on the source. The clump densities range from
~3 10^5-10^6 cm^{-3}, and the sizes and volume filling factors of the clumps
are ~(1-3) 10^{-3} pc and ~0.03-0.12. The clumps are surrounded by inter-clump
gas with densities not lower than ~(2-7) 10^4 cm^{-3}. The internal thermal
energy of the gas in the model clumps is much higher than their gravitational
energy. Their mean lifetimes can depend on the inter-clump collisional rates,
and vary in the range ~10^4-10^5 yr. These structures are probably connected
with density fluctuations due to turbulence in high-mass star-forming regions.Comment: 23 pages including 4 figures and 4 table
PRS46 Tecepoc Study. How to Improve the Inhalation Techniques in Patient with COPD. The Influence of Preferences
The ISLAndS project II: The Lifetime Star Formation Histories of Six Andromeda dSphs
The Initial Star formation and Lifetimes of Andromeda Satellites (ISLAndS)
project uses Hubble Space Telescope imaging to study a representative sample of
six Andromeda dSph satellite companion galaxies. The main goal of the program
is to determine whether the star formation histories (SFHs) of the Andromeda
dSph satellites demonstrate significant statistical differences from those of
the Milky Way, which may be attributable to the different properties of their
local environments. Our observations reach the oldest main sequence turn-offs,
allowing a time resolution at the oldest ages of ~ 1 Gyr, which is comparable
to the best achievable resolution in the MW satellites. We find that the six
dSphs present a variety of SFHs that are not strictly correlated with
luminosity or present distance from M31. Specifically, we find a significant
range in quenching times (lookback times from 9 to 6 Gyr), but with all
quenching times more than ~ 6 Gyr ago. In agreement with observations of Milky
Way companions of similar mass, there is no evidence of complete quenching of
star formation by the cosmic UV background responsible for reionization, but
the possibility of a degree of quenching at reionization cannot be ruled out.
We do not find significant differences between the SFHs of the three members of
the vast, thin plane of satellites and the three off-plane dSphs. The primary
difference between the SFHs of the ISLAndS dSphs and Milky Way dSph companions
of similar luminosities and host distances is the absence of very late
quenching (< 5 Gyr ago) dSphs in the ISLAndS sample. Thus, models that can
reproduce satellite populations with and without late quenching satellites will
be of extreme interest.Comment: 24 pages, 11 figures, 3 tables, submitted to the Ap
Why royalties ? Evidence from French distribution networks
Working paper GATE 2011-02This empirical note deals with the contractual design of relationships in distribution networks. In the framework of agency theory, I study the royalty rate as an incentive device for the upstream firm in maintaining brand-name value, using recent French data to estimate probit models. The results are consistent with the analytical framework
Fabrication and Actuation of Magnetic Shape-Memory Materials
Soft actuators are deformable materials that change their dimensions and/or shape in response to external stimuli. Among the various stimuli, remote magnetic fields are one of the most attractive forms of actuation, due to their ease of use, fast response and safety in biological systems. Composites of magnetic particles with polymer matrices are the most common material for magnetic soft actuators. In this paper, we demonstrate the fabrication and actuation of magnetic shape-memory materials based on hydrogels containing field-structured magnetic particles. These actuators are formed by placing the pregel dispersion into a mold of the desired on-field shape and exposing this to a homogeneous magnetic field until the gel point is reached. At this point the material may be removed from the mold and fully gelled in the desired off-field shape. The resultant magnetic shape-memory material then transitions between these two shapes when subjected to successive cycles of a homogeneous magnetic field, acting as a large deformation actuator. For actuators that are planar in the off-field state, this can result in significant bending to return to the on-field state. In addition, it is possible to make shape-memory materials that twist under the application of a magnetic field. For these torsional actuators, both experimental and theoretical results are given.Departamento de Física AplicadaGrupo FQM144Ministerio de Ciencia, Innovación y UniversidadesAgencia Estatal de InvestigaciónDeutsche Forschungsgemeinschaft (DFG
Rapid Formation of Molecular Clouds and Stars in the Solar Neighborhood
Observations of both star-forming regions and young, gas-free stellar
associations indicate that most nearby molecular clouds form stars only over a
short time span before dispersal; large-scale flows in the diffuse interstellar
medium have the potential for forming clouds sufficiently rapidly, and for
producing stellar populations with ages much less than the lateral crossing
times of their host molecular clouds. We identify four important factors for
understanding rapid star formation and short cloud lifetimes. First, much of
the accumulation and dispersal of clouds near the solar circle might occur in
the atomic phase; only the high-density portion of a cloud's lifecycle is spent
in the molecular phase, thus helping to limit molecular cloud ``lifetimes''.
Second, once a cloud achieves a high enough column density to form \h2 and
CO, gravitational forces become larger than typical interstellar pressure
forces; thus star formation can follow rapidly upon molecular gas formation and
turbulent dissipation in limited areas of each cloud complex. Third, typical
magnetic fields are not strong enough to prevent rapid cloud formation and
gravitational collapse. Fourth, rapid dispersal of gas by newly-formed stars,
and reduction of shielding by a small expansion of the cloud after the first
events of star formation, might limit the length of the star formation epoch
and the lifetime of a cloud in its molecular state. This picture emphasizes the
importance of large-scale boundary conditions for understanding molecular cloud
formation, and implies that star formation is a highly dynamic, rather than
quasi-static, process.Comment: 41 pages, 10 figures, accepted by Ap
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