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. 2017 Nov 29;20(1):7. doi: 10.1007/s41114-017-0008-x

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© The Author(s) 2017

Open AccessThis article is distributed under the terms of the Creative Commons Attribution 4.0 International License (http://creativecommons.org/licenses/by/4.0/), which permits unrestricted use, distribution, and reproduction in any medium, provided you give appropriate credit to the original author(s) and the source, provide a link to the Creative Commons license, and indicate if changes were made.

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Fig. 20 — Evolution of the axial velocity in the equatorial plane for a relativistic r-mode in a rapidly rotating $N = 1.0$ polytrope (in the Cowling approximation). Since the initial data used to excite the mode are not exact, the evolution is a superposition of (mainly) the $l = m = 2$ r-mode and several inertial modes. The amplitude of the oscillation decreases due to numerical (finite-differencing) viscosity of the code. A beating between the $l = m = 2$ r-mode and another inertial mode can also be seen. (Image reproduced with permission from Stergioulas and Font 2001, copyright by APS)