23,561 research outputs found
catena-Poly[[[diaquacopper(II)]-bis[μ-1,1′-(butane-1,4-diyl)diimidazole-κ2 N 3:N 3′]] dinitrate]
In the title compound, {[Cu(C10H14N4)2(H2O)2](NO3)2}n, the CuII ion lies on an inversion center and is six-coordinated in an octahedral environment by four N atoms from four different 1,1′-butane-1,4-diyldiimidazole ligands and two O atoms from the two water molecules. Bridging by the ligands results in a ribbon structure. Adjacent ribbons are linked to the nitrate anions via O—H⋯O hydrogen bonds, forming layers. One nitrate O atom is disordered equally over two positions
Two dimensional numerical simulations of Supercritical Accretion Flows revisited
We study the dynamics of super-Eddington accretion flows by performing
two-dimensional radiation-hydrodynamic simulations. Compared with previous
works, in this paper we include the component of the viscous
stress and consider various values of the viscous parameter . We find
that when is included, the rotational speed of the
high-latitude flow decreases, while the density increases and decreases at the
high and low latitudes, respectively. We calculate the radial profiles of
inflow and outflow rates. We find that the inflow rate decreases inward,
following a power law form of . The value of
depends on the magnitude of and is within the range of .
Correspondingly, the radial profile of density becomes flatter compared with
the case of a constant . We find that the density profile can be
described by , and the value of is almost same for a
wide range of ranging from to . The inward
decrease of inflow accretion rate is very similar to hot accretion flows, which
is attributed to the mass loss in outflows. To study the origin of outflow, we
analyze the convective stability of slim disk. We find that depending on the
value of , the flow is marginally stable (when is small) or
unstable (when is large). This is different from the case of
hydrodynamical hot accretion flow where radiation is dynamically unimportant
and the flow is always convectively unstable. We speculate that the reason for
the difference is because radiation can stabilize convection. The origin of
outflow is thus likely because of the joint function of convection and
radiation, but further investigation is required.Comment: 16 pages, 13 figures, accepted for publication in Ap
Statistics of Chaotic Resonances in an Optical Microcavity
Distributions of eigenmodes are widely concerned in both bounded and open
systems. In the realm of chaos, counting resonances can characterize the
underlying dynamics (regular vs. chaotic), and is often instrumental to
identify classical-to-quantum correspondence. Here, we study, both
theoretically and experimentally, the statistics of chaotic resonances in an
optical microcavity with a mixed phase space of both regular and chaotic
dynamics. Information on the number of chaotic modes is extracted by counting
regular modes, which couple to the former via dynamical tunneling. The
experimental data are in agreement with a known semiclassical prediction for
the dependence of the number of chaotic resonances on the number of open
channels, while they deviate significantly from a purely
random-matrix-theory-based treatment, in general. We ascribe this result to the
ballistic decay of the rays, which occurs within Ehrenfest time, and
importantly, within the timescale of transient chaos. The present approach may
provide a general tool for the statistical analysis of chaotic resonances in
open systems.Comment: 5 pages, 5 figures, and a supplemental informatio
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