Dissipation quality factor normalized to the size of the planet for Jupiter-like and Saturn-like giant planets. Note that all curves are represented on a logarithmic scale. Left: dependence on the perturbative strain pulsation ω, with R_c =  { 0.17,0.26 }  × R_p. Right: dependence on the size of the core, with ω ≃ 2.25 × 10^-4   rad   s^-1 (tidal frequency of Enceladus) for the blue curve associated with a Saturn-like planet, and ω ≃ 2.79 × 10^-4   rad   s^-1 (tidal frequency of Io) for the red curve associated with a Jupiter-like planet. The green curve corresponds to the prescription of Goodman & Lackner (2009) (see plain text for details). The red and blue dashed lines correspond to the value of (for Jupiter and Saturn, respectively) determined by Lainey et al. (2009–2012). Their zone of uncertainty is also represented by the corresponding color. We assume the values of R_p =  { 10.97,9.14 }  (in units of ), M_p =  { 317.8,95.16 }  (in units of ), and given in Tables 5, 6. We also assume the viscoelastic parameters, for Jupiter and Saturn respectively, G =  { 4.85,4.45 }  × 10¹⁰   (Pa), and η =  { 1.26,1.78 }  × 10¹⁴   (Pa   s).