The process of tidal dissipation inside Jupiter is not yet understood .
Its tidal quality factor ( Q ) is inferred to lie between 10 ^ { 5 } and 10 ^ { 6 } .
Having studied the structure and properties of inertial-modes in a neutrally buoyant , core-less , uniformly rotating sphere ( 31 ) , we examine here their effects on tidal dissipation .
The rate of dissipation caused by resonantly excited inertial-modes depends on the following three parameters : how well they are coupled to the tidal potential , how strongly they are dissipated ( by the turbulent viscosity ) , and how densely distributed they are in frequency .
We find that as a function of tidal frequency , the Q value exhibits large fluctuations , with its maximum value set by the group of inertial-modes that satisfy \delta \omega \sim \gamma , where \delta \omega is the group ’ s typical offset from an exact resonance , and \gamma their turbulent damping rates .
These are intermediate order inertial-modes with wave-number \lambda \sim 60 and they are excited to a small surface displacement amplitude of order 10 ^ { 3 } cm .
The Q value drops much below the maximum value whenever a lower order mode happens to be in resonance .
In our model , inertial-modes shed their tidally acquired energy very close to the surface within a narrow latitudinal zone ( the ’ singularity belt ’ ) , and the tidal luminosity escapes freely out of the planet .

Strength of coupling between the tidal potential and inertial-modes is sensitive to the presence of density discontinuities inside Jupiter .
In the case of a discreet density jump , as may be caused by the transition between metallic and molecular hydrogen , we find a time-averaged Q \sim 10 ^ { 7 } , with a small but non-negligible chance ( \sim 10 \% ) that the current Q value falls within the empirically determined range .
Whereas when such a jump does not exist , Q \sim 10 ^ { 9 } .
Even though it remains unclear whether tidal dissipation due to resonant inertial-modes is the correct answer to the problem , it is impressive that our simple treatment here already leads to three to five orders of magnitude stronger damping than that from the equilibrium tide .

Moreover , our conclusions are not affected by the presence of a small solid core , a different prescription for the turbulent viscosity , or nonlinear mode coupling , but they depend critically on the static stability in the upper atmosphere of Jupiter .
This is currently uncertain .
Lastly , we compare our results with those from a competing work by Ogilvie & Lin ( 19 ) and discuss the prospect of extending this theory to exo-jupiters , which appear to possess Q values similar to that of Jupiter .