r-Mode in Young Neutron Stars
[Drawn from Lindblom, Tohline & Vallisneri (2001a,b)]

Simulation Technique
CACR: HP Exemplar
Initial Equilibrium Configuration
  • HSCF technique
  • Uniformly rotating, n = 1 Polytrope
    (Erot/|Egrav| = 0.10)
  • Perturb model with linearized r-mode velocity field

Simulation Results