The predominant contribution to the frequency splitting of low-ℓ solar p modes arises from the rotation of the solar interior and this lifts the frequency degeneracy in ℓ to give a symmetric pattern where the observed (synodic) separation between adjacent m (i.e., for |Δm| = 1) is ∼ 400 nHz. Magnetic fields can also contribute to the splitting, but they do so in such a way as to introduce asymmetries in the arrangement of the components within each multiplet. In full-disc data this effect may become apparent when ℓ ≥ 2. Here, we extract estimates of the frequency asymmetry for ℓ = 2, investigate variations over the activity cycle and compare the results with the near-surface predictions of Dziembowski et al. (2000) which are based upon observations from higher ℓ.