Potential Vorticity Evolution in the Co-orbital Region of Embedded Protoplanets Page: 75 of 175
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the subsequently self-excited vortices is quite similar to the development of the
Kelvin-Helmholtz (KH) instability observed at shear interfaces.- t=120P
t=80P
t=20P
t=40P
-1I 3 I-
4=
t=0-6 -5 -4 -3 -2 -1
0
Ar [rH]1 2 3 4 5 6
Figure 6.1: Evolution of the azimuthally averaged potential vorticity (C) for c8 =
0.05 at different times t = 0, 20P, 40P, 80P, 120P. Take the structure at Ar ~
2 - 3rH as an example. The profile develops dips (Ar = 2.4rH) and peaks (Ar =
3.4rH) progressively from t = 0 - 80P until the vortices are produced at t = 90P,
after which the minimum flattens (see the bold t = 120P curve).
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Koller, J. Potential Vorticity Evolution in the Co-orbital Region of Embedded Protoplanets, thesis or dissertation, September 1, 2004; Los Alamos, New Mexico. (https://digital.library.unt.edu/ark:/67531/metadc779530/m1/75/: accessed April 18, 2024), University of North Texas Libraries, UNT Digital Library, https://digital.library.unt.edu; crediting UNT Libraries Government Documents Department.