Three-Dimensional Spectrum and Processing of Digital NTSC Color Signals

SMPTE Journal ◽  
1982 ◽  
Vol 91 (4) ◽  
pp. 372-378 ◽  
Author(s):  
E. Dubois ◽  
M. S. Sabri ◽  
J.-Y. Ouellet
Keyword(s):  
Three Dimensional ◽  
Dimensional Spectrum ◽  
Color Signals

scholarly journals IS THE SUN LIGHTER THAN THE EARTH? ISOTOPIC CO IN THE PHOTOSPHERE, VIEWED THROUGH THE LENS OF THREE-DIMENSIONAL SPECTRUM SYNTHESIS

2013 ◽  
Vol 765 (1) ◽  
pp. 46 ◽  
Author(s):  
Thomas R. Ayres ◽  
J. R. Lyons ◽  
H.-G. Ludwig ◽  
E. Caffau ◽  
S. Wedemeyer-Böhm
Keyword(s):  
Three Dimensional ◽  
The Sun ◽  
The Earth ◽  
Dimensional Spectrum ◽  
Spectrum Synthesis

scholarly journals Three-dimensional spectrum of temperature fluctuations in stably stratified atmosphere

2008 ◽  
Vol 26 (7) ◽  
pp. 2037-2042 ◽  
Author(s):  
A. S. Gurvich ◽  
I. P. Chunchuzov
Keyword(s):  
Internal Waves ◽  
Horizontal Plane ◽  
Additional Assumption ◽  
Three Dimensional ◽  
Temperature Fluctuations ◽  
Wave Number ◽  
Axially Symmetric ◽  
Dimensional Spectrum ◽  
Analytic Expressions ◽  
Good Agreement

Abstract. A phenomenological model is proposed for a 3-D spectrum of temperature inhomogeneities generated by internal waves in the atmosphere. This model is a development of the theory based on the assumption that a field of Lagrangian displacements of fluid particles, induced by an ensemble of internal waves with randomly independent amplitudes and phases, is statistically stationary, homogeneous, axially symmetric in horizontal plane and Gaussian. For consistency of this model with measured spectra of temperature fluctuations in the stratosphere and mesosphere the additional assumption was introduced in to the model about the anisotropy of inhomogeneities to be dependent on their vertical sizes. The analytic expressions for both the 3-D and 1-D spectra are obtained. A model vertical wave number spectrum follows a −3 power law, whereas a horizontal spectrum contains two regions with a −3 slope, and the intermediate region with the slope between −1 and −3 depending on the rate of anisotropy decrease as a function of increasing sizes of the inhomogeneities. In the range of a few decades the model showed a good agreement with the results of measurements of the spectra in the troposphere, stratosphere and mesosphere.

Parametric instability in the expanding solar wind

2021 ◽  
Author(s):  
Andrea Verdini ◽  
Roland Grappin ◽  
Francesco Malara ◽  
Leonardo Primavera ◽  
Luca Del Zanna
Keyword(s):  
Magnetic Field ◽  
Solar Wind ◽  
Parametric Instability ◽  
Three Dimensional ◽  
Two Dimensional ◽  
Total Magnetic Field ◽  
One Dimensional ◽  
Preliminary Results ◽  
Dimensional Spectrum ◽  
N Wave

<p>Recent measurments of Parker Solar Probe show that alfvenic fluctuations in the solar wind often appear in the form of swithcback with constant total magnetic field. Our aim is to understand if and how such fluctuations can contribute to the heating or acceleration of the solar wind, via the Parametric Instability. The intability of one dimensional Alfvénic fluctuations has been extensively studied in both homogenoeus plasma and in the expanding solar wind, less so for the two-dimensional case which is closer to expected three-dimensional nature of switchbacks. In this work we study under which condition an Alfvén wave with a two dimensional spectrum (as introduced in Primavera et al ApJ 2019) can decay in the expanding solar wind and we will present preliminary results.</p>

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