The Rotation of the Deep Solar Layers

From the analysis of low-order GOLF+MDI sectoral modes (ℓ ≤ 3, 6 ≤ n ≤ 15, | m | = ℓ) and LOWL data (ℓ > 3), we derive the radial rotation profile by assuming no latitudinal dependence in the solar core. These low-order acoustic modes contain the most statistically significant information about the rotation of the deepest solar layers and should be least influenced by internal variability associated with the solar dynamo. After the correction of the sectoral splittings for their contamination by the rotation of the higher latitudes, we obtain a flat rotation profile down to 0.2 R ☉ .