Poster abstract details

Today, the dynamics and the structure of the solar interior are not yet well constrained. While the sound speed is well determined down to the core thanks to the acoustic modes, specially the l=0 modes, the density is not well constrained. Indeed, the acoustic modes being sensitive to pressure, we can have access to the sound speed profile in the inner core of the Sun. Concerning the density, we need the g modes as they are more sensitive to this quantity.
It has already been shown that adding a few g modes in the rotation inversions can give some information on the trend of the rotation rate in the solar core.
We will show here how these profiles are improved adding several g modes.