2,955 research outputs found
Supercritical multicomponent solvent coal extraction
The yield of organic extract from the supercritical extraction of coal with larger diameter organic solvents such as toluene is increased by use of a minor amount of from 0.1 to 10% by weight of a second solvent such as methanol having a molecular diameter significantly smaller than the average pore diameter of the coal
Coal desulfurization by aqueous chlorination
A method of desulfurizing coal is described in which chlorine gas is bubbled through an aqueous slurry of coal at low temperature below 130 degrees C., and at ambient pressure. Chlorinolysis converts both inorganic and organic sulfur components of coal into water soluble compounds which enter the aqueous suspending media. The media is separated after chlorinolysis and the coal dechlorinated at a temperature of from 300 C to 500 C to form a non-caking, low-sulfur coal product
The three-dimensional structure of the Eta Carinae Homunculus
We investigate, using the modeling code SHAPE, the three-dimensional
structure of the bipolar Homunculus nebula surrounding Eta Carinae, as mapped
by new ESO VLT/X-Shooter observations of the H2 micron
emission line. Our results reveal for the first time important deviations from
the axisymmetric bipolar morphology: 1) circumpolar trenches in each lobe
positioned point-symmetrically from the center and 2) off-planar protrusions in
the equatorial region from each lobe at longitudinal (~55 degrees) and
latitudinal (10-20 degrees) distances from the projected apastron direction of
the binary orbit. The angular distance between the protrusions (~110 degrees)
is similar to the angular extent of each polar trench (~130 degrees) and nearly
equal to the opening angle of the wind-wind collision cavity (~110 degrees). As
in previous studies, we confirm a hole near the centre of each polar lobe and
no detectable near-IR H2 emission from the thin optical skirt seen prominently
in visible imagery. We conclude that the interaction between the outflows
and/or radiation from the central binary stars and their orientation in space
has had, and possibly still has, a strong influence on the Homunculus. This
implies that prevailing theoretical models of the Homunculus are incomplete as
most assume a single star origin that produces an axisymmetric nebula. We
discuss how the newly found features might be related to the Homunculus
ejection, the central binary and the interacting stellar winds. We also include
a 3D printable version of our Homunculus model.Comment: 14 pages, 7 color figures, 1 interactive 3D figure (Figure 5,
requires Adobe Reader), published in MNRAS. A 3D printable version of our
Homunculus model can be downloaded from
http://svs.gsfc.nasa.gov/vis/a010000/a011500/a011568/Eta_Car_Homunuculus_3D_model.zip
or from the 'Supporting Information' link in the electronic version of the
MNRAS articl
aristotle's demonstrative logic
Demonstrative logic, the study of demonstration as opposed to persuasion, is the subject of Aristotle's two-volume Analytics. Many examples are geometrical. Demonstration produces knowledge (of the truth of propositions). Persuasion merely produces opinion. Aristotle presented a general truth-and-consequence conception of demonstration meant to apply to all demonstrations. According to him, a demonstration, which normally proves a conclusion not previously known to be true, is an extended argumentation beginning with premises known to be truths and containing a chain of reasoning showing by deductively evident steps that its conclusion is a consequence of its premises. In particular, a demonstration is a deduction whose premises are known to be true. Aristotle's general theory of demonstration required a prior general theory of deduction presented in the Prior Analytics. His general immediate-deduction-chaining conception of deduction was meant to apply to all deductions. According to him, any deduction that is not immediately evident is an extended argumentation that involves a chaining of intermediate immediately evident steps that shows its final conclusion to follow logically from its premises. To illustrate his general theory of deduction, he presented an ingeniously simple and mathematically precise special case traditionally known as the categorical syllogisti
Reorientation of magnetic anisotropy in epitaxial cobalt ferrite thin films
Spin reorientation has been observed in CoFe2O4 thin single crystalline films epitaxially grown on (100) MgO substrate upon varying the film thickness. The critical thickness for such a spin-reorientation transition was estimated to be 300 nm. The reorientation is driven by a structural transition in the film from a tetragonal to cubic symmetry. At low thickness, the in-plane tensile stress induces a tetragonal distortion of the lattice that generates a perpendicular anisotropy, large enough to overcome the shape anisotropy and to stabilize the magnetization easy axis out of plane. However, in thicker films, the lattice relaxation toward the cubic structure of the bulk allows the shape anisotropy to force the magnetization to be in plane aligned
Analysis and contribution of stress anisotropy in epitaxial hard ferrite thin films
The stress anisotropy in epitaxial hard ferrites thin films (BaFe12O19, CoFe2O4) has been investigated using two methods. (a) The thickness dependence of torque curves and magnetic hysteresis loops. (b) The comparison between magnetic and magneto-optic Kerr hysteresis loops. Both analyses confirm the domination of stress in CoFe2O4 whereas in BaFe12O19 films the stress is too weak to compete with magnetocrystalline anisotropy
Coherence in the Quasi-Particle 'Scattering' by the Vortex Lattice in Pure Type-II Superconductors
The effect of quasi-particle (QP) 'scattering' by the vortex lattice on the
de-Haas van-Alphen oscillations in a pure type-II superconductor is
investigated within mean field,asymptotic perturbation theory. Using a 2D
electron gas model it is shown that, due to a strict phase coherence in the
many-particle correlation functions, the 'scattering' effect in the asymptotic
limit () is much weaker than what is predicted
by the random vortex lattice model proposed by Maki and Stephen, which destroys
this coherence . The coherent many particle configuration is a collinear array
of many particle coordinates, localized within a spatial region with size of
the order of the magnetic length. The amplitude of the magnetization
oscillations is sharply damped just below because of strong
out of phase magnetic oscillations in the superconducting
condensation energy ,which tend to cancel the normal electron oscillations.
Within the ideal 2D model used it is found, however, that because of the
relative smallness of the quartic and higher order terms in the expansion, the
oscillations amplitude at lower fields does not really damp to zero, but only
reverses sign and remains virtually undamped well below . This
conclusion may be changed if disorder in the vortex lattice, or vortex lines
motion will be taken into account. The reduced QP 'scattering' effect may be
responsible for the apparent crossover from a strong damping of the dHvA
oscillations just below to a weaker damping at lower fields observed
experimentally in several 3D superconductors.Comment: 26 pages, Revtex no Figure
Chandra X-ray Spectroscopic Imaging of Sgr A* and the Central Parsec of the Galaxy
We present results of our Chandra observation with the ACIS-I instrument
centered on the position of Sagittarius A* (Sgr A*), the compact nonthermal
radio source associated with the massive black hole (MBH) at the dynamical
center of the Milky Way Galaxy. We have obtained the first
high-spatial-resolution (~1 arcsec), hard X-ray (0.5-7 keV) image of the
central 40 pc (17 arcmin) of the Galaxy and have discovered an X-ray source,
CXOGC J174540.0-290027, coincident with the radio position of Sgr A* to within
0.35 arcsec, corresponding to a maximum projected distance of 16 light-days for
an assumed distance to the center of the Galaxy of 8.0 kpc. We received 222
+/-17 (1 sigma) net counts from the source in 40.3 ks. Due to the low number of
counts, the spectrum is well fit either by an absorbed power-law model with
photon index Gamma = 2.7 (1.8-4.0) and column density NH = (9.8 [6.8-14.2]) x
10^22 cm^-2 (90% confidence interval) or by an absorbed optically thin thermal
plasma model with kT = 1.9 (1.4-2.8) keV and NH = (11.5 [8.4-15.9]) x 10^22
cm^-2. Using the power-law model, the measured (absorbed) flux in the 2-10 keV
band is (1.3 [1.1-1.7]) x 10^-13 ergs cm^-2 s^-1, and the absorption-corrected
luminosity is (2.4 [1.8-5.4]) x 10^33 ergs s^-1. We also briefly discuss the
complex structure of the X-ray emission from the Sgr A radio complex and along
the Galactic plane and present morphological evidence that Sgr A* and Sgr A
West lie within the hot plasma in the central cavity of Sgr A East.Comment: 33 pages, 10 figures (Figures 2-5 in color), LaTeX, emulateapj5.sty,
submitted to The Astrophysical Journal, version with full-resolution figures
available at http://space.mit.edu/~fkb/GC
A Coordinated X-ray and Optical Campaign of the Nearby Massive Binary Orionis Aa: II. X-ray Variability
We present time-resolved and phase-resolved variability studies of an
extensive X-ray high-resolution spectral dataset of the Orionis Aa
binary system. The four observations, obtained with Chandra ACIS HETGS, have a
total exposure time of ~479 ks and provide nearly complete binary phase
coverage. Variability of the total X-ray flux in the range 5-25 is
confirmed, with maximum amplitude of about +/-15% within a single ~125 ks
observation. Periods of 4.76d and 2.04d are found in the total X-ray flux, as
well as an apparent overall increase in flux level throughout the 9-day
observational campaign. Using 40 ks contiguous spectra derived from the
original observations, we investigate variability of emission line parameters
and ratios. Several emission lines are shown to be variable, including S XV, Si
XIII, and Ne IX. For the first time, variations of the X-ray emission line
widths as a function of the binary phase are found in a binary system, with the
smallest widths at phase=0.0 when the secondary Orionis Aa2 is at
inferior conjunction. Using 3D hydrodynamic modeling of the interacting winds,
we relate the emission line width variability to the presence of a wind cavity
created by a wind-wind collision, which is effectively void of embedded wind
shocks and is carved out of the X-ray-producing primary wind, thus producing
phase-locked X-ray variability.Comment: 36 pages, 14 Tables, 19 Figures, accepted by ApJ, one of 4 related
papers to be published togethe
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