A Method to Easily Visualize and Solve a Convolution Integral by Direct Integration

2011 ◽  
Author(s):  
Rodolfo E. Firpo

2021 ◽  
Vol 19 (11) ◽  
pp. 2473-2480
Author(s):  
Jigarkumar K. Vankar ◽  
Ankush Gupta ◽  
Jaydeepbhai P. Jadav ◽  
Shankara H. Nanjegowda ◽  
Guddeangadi N. Gururaja

The direct integration of sulphur and amine groups with 1,1-dibromoalkenes for thioamide synthesis has been achieved in an aqueous medium.



2021 ◽  
Vol 182 ◽  
pp. 411-427
Author(s):  
Nadirah Mohd Nasir ◽  
Zanariah Abdul Majid ◽  
Fudziah Ismail ◽  
Norfifah Bachok




Author(s):  
Rehab M. El-Shiekh ◽  
Mahmoud Gaballah

AbstractIn this paper, the generalized nonlinear Schrödinger equation with variable coefficients (gvcNLSE) arising in optical fiber is solved by using two different techniques the trail equation method and direct integration method. Many different new types of wave solutions like Jacobi, periodic and soliton wave solutions are obtained. From this study we have concluded that the direct integration method is more easy and straightforward than the trail equation method. As an application in optic fibers the propagation of the frequency modulated optical soliton is discussed and we have deduced that it's propagation shape is affected with the different values of both the amplification increment and the group velocity (GVD).



2010 ◽  
Vol 181 (21-22) ◽  
pp. 1009-1014
Author(s):  
Chang-Mook Lee ◽  
Jaewu Choi


2013 ◽  
Vol 8 (S300) ◽  
pp. 265-268
Author(s):  
Miho Janvier ◽  
Pascal Démoulin ◽  
Sergio Dasso

AbstractMagnetic clouds (MCs) consist of flux ropes that are ejected from the low solar corona during eruptive flares. Following their ejection, they propagate in the interplanetary medium where they can be detected by in situ instruments and heliospheric imagers onboard spacecraft. Although in situ measurements give a wide range of data, these only depict the nature of the MC along the unidirectional trajectory crossing of a spacecraft. As such, direct 3D measurements of MC characteristics are impossible. From a statistical analysis of a wide range of MCs detected at 1 AU by the Wind spacecraft, we propose different methods to deduce the most probable magnetic cloud axis shape. These methods include the comparison of synthetic distributions with observed distributions of the axis orientation, as well as the direct integration of observed probability distribution to deduce the global MC axis shape. The overall shape given by those two methods is then compared with 2D heliospheric images of a propagating MC and we find similar geometrical features.



2011 ◽  
Vol 26 (12) ◽  
pp. 3720-3729 ◽  
Author(s):  
S. D. Gamini Jayasinghe ◽  
D. Mahinda Vilathgamuwa ◽  
Udaya K. Madawala


1989 ◽  
Vol 163 (2) ◽  
pp. 1086-1092 ◽  
Author(s):  
Tadashi Yoshida ◽  
Michihiko Sato


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