Figure 4 - uploaded by James Beattie
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A visualisation of the predictions made from our M − D relation (Equation 4) on a single time slice of the log mean column density from the M = 4 simulation. We show regions of the cloud in blue boxes that are undergoing turbulent motions from M = 1 to M = 4, in 0.5M increments, indicated by the label in the corner of each of the boxes. Our method uses wrap-around boundaries, so the /L × /L region wraps around the simulation data as it expands. We initialise our method at the maximum column density, Σ max. The code for our method is publicly accessible, from: https://jrbeatti@bitbucket.org/jrbeatti/fractal-dimension-spectrum

A visualisation of the predictions made from our M − D relation (Equation 4) on a single time slice of the log mean column density from the M = 4 simulation. We show regions of the cloud in blue boxes that are undergoing turbulent motions from M = 1 to M = 4, in 0.5M increments, indicated by the label in the corner of each of the boxes. Our method uses wrap-around boundaries, so the /L × /L region wraps around the simulation data as it expands. We initialise our method at the maximum column density, Σ max. The code for our method is publicly accessible, from: https://jrbeatti@bitbucket.org/jrbeatti/fractal-dimension-spectrum

Source publication
Poster
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The turbulent Mach number of molecular clouds (M) plays an important role in star formation. Mach numbers are typically estimated using optically thin molecular lines, however these measurements are sensitive to complex chemistry in the cloud, and the light-absorbing properties of the cloud. In this poster we present a novel method for calculating...

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