Apparatus for stoage of filamentary material

Composites ◽  
1977 ◽  
Vol 8 (4) ◽  
pp. 267
Keyword(s):  
Filamentary Material

Some Problems in Winding Geometry

1981 ◽  
Vol 103 (4) ◽  
pp. 418-423 ◽  
Author(s):  
M. M. Schoppee
Keyword(s):  
Reverse Osmosis ◽  
Flow Rate ◽  
Hollow Fiber ◽  
Cross Sectional ◽  
Core Flow ◽  
Fiber Separation ◽  
Helical Winding ◽  
Module Geometry ◽  
Analytical Requirements ◽  
Filamentary Material

The efficiency of wound, hollow-fiber separation modules used to remove dissolved salts from water by the process of reverse osmosis may be improved by alterations in module geometry. Normally, the hollow-fiber membranes composing the module are helically wound about a cylindrical core. Flow rate through the module may be increased, however, if the cross-sectional density of wound fibers varies uniformly along the module axis. This paper explores the analytical requirements for the helical winding of a conical mandrel with filamentary material in a manner that eventually produces a cylindrically shaped package. The effect of specifying either a constant yarn feed rate or a constant spindle speed during winding is considered in relation to restrictions on the length of material added per circuit.

scholarly journals Modeling high-redshift galaxies: what can we learn from high and ultra-high resolution hydrodynamical simulations?

2009 ◽  
Vol 5 (S262) ◽  
pp. 248-256
Author(s):  
J. Devriendt ◽  
A. Slyz ◽  
L. Powell ◽  
C. Pichon ◽  
R. Teyssier
Keyword(s):  
High Resolution ◽  
Galaxy Formation ◽  
Globular Clusters ◽  
High Redshift ◽  
Cosmological Parameters ◽  
High Redshift Galaxies ◽  
Luminosity Functions ◽  
Hydrodynamical Simulations ◽  
Consistent Treatment ◽  
Filamentary Material

AbstractWe present results from a high resolution cosmological galaxy formation simulation called Mare Nostrum and a ultra-high resimulation of the first 500 million years of a single, Milky Way (MW) sized galaxy. Using the cosmological run, we measure UV luminosity functions and assess their sensitivity to both cosmological parameters and dust extinction. We find remarkably good agreement with the existing data over the redshift range 4 < z < 7 provided we adopt the favoured cosmology (WMAP 5 year parameters) and a self-consistent treatment of the dust. Cranking up the resolution, we then study in detail a z = 9 protogalaxy sitting at the intersection of cold gas filaments. This high-z MW progenitor grows a dense, rapidly spinning, thin disk which undergoes gravitational fragmention. Star formation in the resulting gas clumps rapidly turns them into globular clusters. A far reaching galactic wind develops, co-powered by the protogalaxy and its cohort of smaller companions populating the filaments. Despite such an impressive blow out, the smooth filamentary material is hardly affected at these redshifts.

Electrostatic charge of filamentary material

2004 ◽  
Vol 36 (5) ◽  
pp. 379-382
Author(s):  
I. D. Pupyshev ◽  
O. I. Kolerova
Keyword(s):  
Electrostatic Charge ◽  
Filamentary Material

scholarly journals Active Regions at Millimeter Wavelengths and the Measurement of Magnetic Fields

1971 ◽  
Vol 43 ◽  
pp. 642-651 ◽  
Author(s):  
M. R. Kundu
Keyword(s):  
Magnetic Fields ◽  
Electron Density ◽  
Optical Thickness ◽  
Background Radiation ◽  
Active Regions ◽  
Brightness Temperatures ◽  
Millimeter Wavelengths ◽  
Solar Active Regions ◽  
Large Optical Thickness ◽  
Filamentary Material

Some properties of solar active regions at 9 and 3.5 mm wavelengths are discussed. The regions have excess brightness temperatures of up to 1000 and 700K at 9 and 3.5 mm wavelengths respectively. The background radiation at 3.5 mm is often seen to be ‘absorbed’ in regions closely coincident with Hα dark filaments on the disk. Interpretation of this ‘absorption’ as due to the large optical thickness of the overlying filamentary material leads to an estimate of electron density in the filaments. The active regions at millimeter wavelengths show almost one-to-one correspondence with the Ca-plage regions as well as with the regions of longitudinal magnetic fields on Mt. Wilson magnetograms. A comparison of the mm-λ maps with the magnetograms ‘smoothed’ with the beams of mm observations shows this correspondence in a striking manner. This relationship suggests the possibility of measuring chromospheric magnetic fields from the measurement of polarization at millimeter wavelengths.

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