scholarly journals A CASE STUDY OF SMALL-SCALE STRUCTURE FORMATION IN THREE-DIMENSIONAL SUPERNOVA SIMULATIONS

2012 ◽  
Vol 755 (2) ◽  
pp. 160 ◽  
Author(s):  
Carola I. Ellinger ◽  
Patrick A. Young ◽  
Christopher L. Fryer ◽  
Gabriel Rockefeller
Keyword(s):  
Structure Formation ◽  
Three Dimensional ◽  
Scale Structure ◽  
Small Scale ◽  
Small Scale Structure

Small-scale structure of two-dimensional magnetohydrodynamic turbulence

1979 ◽  
Vol 90 (1) ◽  
pp. 129-143 ◽  
Author(s):  
Steven A. Orszag ◽  
Cha-Mei Tang
Keyword(s):  
Numerical Simulation ◽  
Direct Numerical Simulation ◽  
Three Dimensional ◽  
Scale Structure ◽  
Magnetohydrodynamic Flow ◽  
Small Scale ◽  
Two Dimensional ◽  
Magnetohydrodynamic Turbulence ◽  
Hydrodynamic Turbulence ◽  
Small Scale Structure

The formation of singularities in two-dimensional magnetohydrodynamic flow is investigated by direct numerical simulation. It is shown that two-dimensional magnetohydrodynamic turbulence is not as singular as three-dimensional hydrodynamic turbulence (in the sense that it has a less highly excited small-scale structure) but that it is more singular than two-dimensional hydrodynamic turbulence.

scholarly journals Small scale structure formation in chameleon cosmology

2006 ◽  
Vol 633 (4-5) ◽  
pp. 441-446 ◽  
Author(s):  
Ph. Brax ◽  
C. van de Bruck ◽  
A.C. Davis ◽  
A.M. Green
Keyword(s):  
Structure Formation ◽  
Scale Structure ◽  
Small Scale ◽  
Small Scale Structure

scholarly journals A Search for Very Compact Structure in 17 OH Masers

1988 ◽  
Vol 129 ◽  
pp. 255-256
Author(s):  
A. J. Kemball ◽  
P. J. Diamond ◽  
F. Mantovani
Keyword(s):  
Galactic Disk ◽  
Hii Regions ◽  
Scale Structure ◽  
Small Scale ◽  
Compact Structure ◽  
Small Scale Structure ◽  
Interstellar Scattering

The apparent spot sizes of OH masers appear to be significantly broadened when seen through the inner galaxy or large extents of the galactic disk (Burke 1968). Bowers et al (1980) found evidence of small-scale structure (≲ 50 mas) in OH sources at distances of less than 5 kpc but this was characteristically absent in very distant sources (≳ 8kpc) at galactic longitudes 1 ≲ 40°. This result is typically explained in terms of interstellar scattering (ISS) by intervening diffuse HII regions.

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