scholarly journals A non-local shell model of hydrodynamic and magnetohydrodynamic turbulence

2007 ◽  
Vol 9 (8) ◽  
pp. 294-294 ◽  
Author(s):  
F Plunian ◽  
R Stepanov
1990 ◽  
Vol 52 (1-3) ◽  
pp. 153-181 ◽  
Author(s):  
Vincenzo Carbone ◽  
Pierluigi Veltri

1971 ◽  
Vol 166 (2) ◽  
pp. 330-340 ◽  
Author(s):  
R.C. Grimm ◽  
I.E. McCarthy ◽  
R.G. Storer

Author(s):  
Archana Saxena ◽  
Praveen C Srivastava

Abstract We have calculated the energy spectra for neutron-rich $^{18-22}$N isotopes using the no-core shell model. To calculate the energy spectrum we have used three different $NN$ potentials: inside non-local outside Yukawa (INOY), next-to-next-to-next-leading order (N3LO) from chiral effective field theory, and charge-dependent Bonn 2000 (CDB2K). The INOY potential is a two-body interaction but also has the effect of three-body forces at short range and a non-local character present in it. The calculations have been done at $\hbar\Omega=20$ MeV, 14 MeV, and 12 MeV using INOY, N3LO, and CDB2K potentials, respectively. We have also performed shell model calculations with the YSOX interaction. The results with the INOY interaction show good agreement with the experimental data in comparison to the other three interactions. We have also shown the occupancy of different orbitals involved corresponding to the largest model space ($N_{\rm max} = 4$) in the calculations.


2013 ◽  
Vol 111 (17) ◽  
Author(s):  
Debarghya Banerjee ◽  
Samriddhi Sankar Ray ◽  
Ganapati Sahoo ◽  
Rahul Pandit

2007 ◽  
Vol 575 ◽  
pp. 111-120 ◽  
Author(s):  
T. A. YOUSEF ◽  
F. RINCON ◽  
A. A. SCHEKOCHIHIN

This paper examines the consistency of the exact scaling laws for isotropic magnetohydrodynamic (MHD) turbulence in numerical simulations with large magnetic Prandtl numbers Pm and with Pm = 1. The exact laws are used to elucidate the structure of the magnetic and velocity fields. Despite the linear scaling of certain third-order correlation functions, the situation is not analogous to the case of Kolmogorov turbulence. The magnetic field is adequately described by a model of a stripy (folded) field with direction reversals at the resistive scale. At currently available resolutions, the cascade of kinetic energy is short-circuited by the direct exchange of energy between the forcing-scale motions and the stripy magnetic fields. This non-local interaction is the defining feature of isotropic MHD turbulence.


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