r-Mode in Young Neutron Stars
[Drawn from Lindblom, Tohline & Vallisneri (2001a,b)]
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Simulation Technique
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CACR: HP Exemplar
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Initial Equilibrium Configuration
- HSCF technique
- Uniformly rotating, n = 1 Polytrope
(Erot/|Egrav| = 0.10)
- Perturb model with linearized r-mode velocity field
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Simulation Results
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