A dimensional decomposition method for stochastic fracture mechanics

2006 ◽  
Vol 73 (15) ◽  
pp. 2093-2109 ◽  
Author(s):  
Sharif Rahman
Keyword(s):  
Fracture Mechanics ◽  
Decomposition Method ◽  
Dimensional Decomposition

scholarly journals Evaluation of Sector Wise Energy Saving and Energy Rebound Effect in Bangladesh by Three Dimensional Decomposition Method

2010 ◽  
Vol 5 (2) ◽  
pp. 85-91 ◽  
Author(s):  
Shaikh Khosruzzam ◽  
M. Ali Asgar ◽  
Naimul Karim ◽  
M. Arif Asgar ◽  
Shawkat Akbar
Keyword(s):  
Energy Saving ◽  
Decomposition Method ◽  
Rebound Effect ◽  
Three Dimensional ◽  
Dimensional Decomposition

scholarly journals 2.8. Two dimensional decomposition of the luminosity distribution of the spiral galaxies : ESO598-G009, NGC1515 and NGC7456

1998 ◽  
Vol 184 ◽  
pp. 73-74
Author(s):  
Young-Jun Choi ◽  
Byeong-Gon Park ◽  
Tae Seog Yoon ◽  
Hong Bae Ann
Keyword(s):  
Decomposition Method ◽  
Spiral Galaxies ◽  
Two Dimensional ◽  
Spiral Arms ◽  
One Dimensional ◽  
Dimensional Decomposition

Because it is inevitable to lose some information in the process of one dimensional luminosity profile extraction, we developed a two dimensional luminosity decomposition method in order to examine the structure of galaxy such as bulge, bar and spiral arms.

scholarly journals The Shape of the Luminosity Profiles of Bulges

1996 ◽  
Vol 157 ◽  
pp. 86-87 ◽  
Author(s):  
Y. Andredakis ◽  
R. Peletier ◽  
M. Balcells
Keyword(s):  
Density Distribution ◽  
Decomposition Method ◽  
Surface Brightness ◽  
A Priori ◽  
Morphological Type ◽  
Early Type ◽  
Late Type ◽  
Dimensional Decomposition ◽  
The Galaxy ◽  
Light Profiles

AbstractWe extract the bulge light profiles of a sample of early type spirals, using K-band photometry and a new 2-dimensional decomposition method that does not assume a priori any surface brightness laws. We find that the shape of the light profile shows a good correlation with the morphological type of the galaxy, in the sense that the profiles tend to fall off more steeply at large radii for the later types. This trend shows that the formation of or interaction with the disk has probably affected the density distribution of the bulge. The fact that the transition in shape is continuous might also imply that most of the bulges of late type spirals were not formed by different mechanisms than the ones of early types.

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