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Characterizing Magnetized Turbulence in M51

  • Authors: Martin Houde, Andrew Fletcher, Rainer Beck, Roger H. Hildebrand, John E. Vaillancourt, and Jeroen M. Stil

Houde et al. 2013 The Astrophysical Journal 766 49.

  • Provider: AAS Journals

Caption: Figure 13.

Top: contour plot of the two-dimensional turbulence autocorrelation function (black) and a Gaussian fit (red); the fit is forced to be even in directions parallel and perpendicular to the mean magnetic field. The contours are drawn at 10%–90% (10% increments) of the peak b 2(0) = 0.063. Bottom: the intrinsic turbulence autocorrelation function, where we set W = 0, α = π/2, and N = 1 in Equations (19) and (21), while using the values for δ || and δ obtained with the Gaussian fit (red) in the plot on the top graph (see Table 3). The contours are drawn at 10%–90% (10% increments) of the peak .

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