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optical density

Definitions

  • WordNet 3.6
    • n optical density (physics) a measure of the extent to which a substance transmits light or other electromagnetic radiation
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Usage

In literature:

This defect in the eye-lens is somewhat counteracted by a variable optical density, increasing from the outer to the central portion.
"Visual Illusions" by Matthew Luckiesh
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In news:

At NAB, Bittree will debut its new SC-to-SC fiber-optic coupler panel, which is designed to simplify high-density patching of fiber connections in rapidly changing media environments.
The new SC-to-SC fiber-optic coupler panel provides 1x24 density in a single rack unit.
As a leading supplier of advanced fiber optic solutions, Molex offers a broad range of high-density products including interconnects and adapters, assemblies, backplanes and more.
Revision of E662 - 12Standard Test Method for Specific Optical Density of Smoke Generated by Solid Materials.
Avago Technologies has released new Active Optical Cable (AOC) family, high density SFP+ QSFP+, and CXP solutions for high performance computing and data centre applications.
At NAB, Bittree will debut its new SC-to-SC fiber- optic coupler panel, which is designed to simplify high-density patching of fiber connections in rapidly changing media environments.
The new SC-to-SC fiber- optic coupler panel provides 1x24 density in a single rack unit.
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In science:

The column densities in each state can be determined from the observed integrated line intensities, assuming they are optically thin.
HCN in the inner envelope of {chi} Cygni
Density of states g (ǫ) of a probe scattered by bosonic atoms in a 1D optical lattice.
Random Scattering by Atomic Density Fluctuations in Optical Lattices
Density-density fluctuations hW 2 i (in units of 10 (neV)2 ) as a function of temperature T for bosonic and fermionic Li atoms in an optical lattice.
Random Scattering by Atomic Density Fluctuations in Optical Lattices
The optical depths in both models are similar, because the density in the n0 = 0.3 cm−3 is smaller, but the thickness of the O VI layer is larger by the same factor because the cooling length increases.
Far Ultraviolet Spectra of a Non-Radiative Shock Wave in the Cygnus Loop
The preliminary results show optical R and V images with a high number density of galaxies.
The Galaxy Cluster RBS380: Xray and Optical Analysis
If such a density profile would still somehow occur, then the observed optical light curve could be reproduced, if the jet would hardly expand sideways at t > tj .
The Variable Light Curve of GRB 030329: The Case for Refreshed Shocks
The density of optical sources in the inner regions of NGC5128 is high, and the positions of the CHANDRA and VLT images are uncertain enough that some spurious matches could be expected.
Optical Counterparts of X-Ray Point Sources Observed by CHANDRA in NGC5128: 20 New Globular Cluster X-Ray Sources
Elliptical galaxies have dominated the total luminosity density in all optical bands at early epochs, when all their stars formed by means of rapid and very intense star-bursts.
The cosmic evolution of the galaxy luminosity density
Detection of the density matrix through optical homodyne tomography without filtered back p rojection.
An invitation to quantum tomography (II)
Measurement of the Wigner distribution and the density matrix of a light mode using optical homodyne tomography: Application to squeezed states and the vacuum.
An invitation to quantum tomography (II)
In this case we used Skyrme-Hartree-Fock model (SKM*) densities to form the g -folding optical potentials.
Simple functional forms for total cross sections from neutron-nucleus collisions
SH and SR are the flux densities in the near-IR H-band and the optical R-band.
Complete Multiwavelength Characterization of Faint Chandra X-ray Sources Seen in the Spitzer Wide-Area IR Extragalactic (SWIRE) Survey
When we combine this with the CMB, we include Ωb h2, the physical baryon density; τ, the optical depth to reionization; T /S the scalar-tensor fluctuation ratio.
Probing decisive answers to dark energy questions from cosmic complementarity and lensing tomography
For example, the uncertain dust optical properties, the unknown dust grain physical status and density distribution, etc.
On the difference between type E and A OH/IR stars
In that case, the lack of such a strong trend in M33 (say, for remnants with SH α ≥ 5×10−14 ergs cm−2 s−1, where only 10 out of 32 optical remnants are detected in the X-rays by Chandra and XMM-Newton) may be partially caused by expansion of the SNRs into regions of lower than average density.
Revealing the Supernova Remnant Population of M33 with Chandra
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