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Turbulence Regulates the Rate of Planetesimal Formation via Gravitational Collapse

  • Authors: Daniel A. Gole, Jacob B. Simon, Rixin Li, Andrew N. Youdin, and Philip J. Armitage

2020 The Astrophysical Journal 904 132.

  • Provider: AAS Journals

Caption: Figure 5.

Power spectrum of the fluid velocity perturbations within a small slice at the midplane for three runs: control (black, αdrive = 0), weak driving (green, αdrive = 10−4), and strong driving (red, αdrive = 10−3). ﹩| {\boldsymbol{k}}| ﹩ is given in code units (1/H). These spectra are compensated such that a power law with an index of −5/3 would appear to be flat. They are normalized by a common factor such that the mean of the control curve is unity. Using this convention, the absolute values of the power bear no meaning, but the relative power between the spectra is maintained. The weak driving and control runs have very similar spectra at small scales but differ on larger scales, which is consistent with small-scale motions being dominated by the presence of a thin particle layer.

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