Two‐dimensional Magnetohydrodynamics and Interstellar Plasma Turbulence

1999 ◽  
Vol 522 (2) ◽  
pp. 879-896 ◽  
Author(s):  
Steven R. Spangler
Keyword(s):  
Plasma Turbulence ◽  
Two Dimensional ◽  
Interstellar Plasma

scholarly journals Interplanetary and interstellar plasma turbulence

2007 ◽  
Vol 49 (5A) ◽  
pp. A195-A209 ◽  
Author(s):  
A A Schekochihin ◽  
S C Cowley ◽  
W Dorland
Keyword(s):  
Plasma Turbulence ◽  
Interstellar Plasma

scholarly journals Local Kinetic Effects in Two-Dimensional Plasma Turbulence

2012 ◽  
Vol 108 (4) ◽  
Author(s):  
S. Servidio ◽  
F. Valentini ◽  
F. Califano ◽  
P. Veltri
Keyword(s):  
Plasma Turbulence ◽  
Two Dimensional ◽  
Kinetic Effects

scholarly journals The Spectrum Power of Interstellar Plasma Inhomogeneities in the Direction of Eleven Radio Pulsars

2021 ◽  
Vol 65 (11) ◽  
pp. 1129-1135
Author(s):  
M. V. Popov ◽  
T. V. Smirnova
Keyword(s):  
Structure Function ◽  
Temporal Structure ◽  
Parameter Estimates ◽  
Archival Data ◽  
Two Dimensional ◽  
Radio Pulsars ◽  
Exponential Functions ◽  
Interstellar Plasma ◽  
Spatial Inhomogeneities ◽  
Better Than

Abstract We have analyzed two-dimensional correlation functions from the dynamic spectra of 11 pulsars using the archival data of the “Radioastron” project. The time-sections of these functions were approximated by exponential functions with a power $$\alpha $$. It is shown that this approximation describes the shape of the correlation function much better than the Gaussian. The temporal structure function $$D(\Delta t)$$ for small values of the delay $$\Delta t$$is a power law with an index $$\alpha $$. The spectrum power of spatial inhomogeneities of the interstellar plasma is related to the power of the structure function as $$n = \alpha + 2$$. We have determined the characteristic scintillation time and the power $$n$$ in the direction of 11 pulsars. In the direction of three pulsars (B0329+54, B0823+26, and B1929+10), the spectrum power of spatial inhomogeneities of the interstellar plasma turned out to be very close to the value for the Kolmogorov spectrum ($$n = 3.67$$). For other pulsars, it ranges from 3.18 to 3.86. It is shown that the measured scintillation parameters are significantly influenced by the duration of the observation session, expressed by its ratio to the characteristic scintillation time. If this parameter is less than 10, the parameter estimates may be biased: the values of $$\alpha $$ and the characteristic scintillation time $${{t}_{{{\text{scint}}}}}$$ may decrease.

scholarly journals Spectral evolution of two-dimensional kinetic plasma turbulence in the wavenumber-frequency domain

2013 ◽  
Vol 20 (9) ◽  
pp. 090701 ◽  
Author(s):  
H. Comişel ◽  
D. Verscharen ◽  
Y. Narita ◽  
U. Motschmann
Keyword(s):  
Frequency Domain ◽  
Plasma Turbulence ◽  
Two Dimensional ◽  
Spectral Evolution

scholarly journals Self-organization and symmetry-breaking in two-dimensional plasma turbulence

2010 ◽  
Vol 17 (9) ◽  
pp. 092302 ◽  
Author(s):  
Wouter J. T. Bos ◽  
Salah Neffaa ◽  
Kai Schneider
Keyword(s):  
Symmetry Breaking ◽  
Plasma Turbulence ◽  
Self Organization ◽  
Two Dimensional
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