Rotational splitting of helioseismic modes influenced by a magnetic atmosphere

In the present paper the splitting of sectoral (m = +/- l) helioseismic eig enmodes (f- andp-modes) is studied in the presence of a magnetic atmosphere . The solar interior is in a steady state, with sub-photospheric plasma ow along the equator representing solar rotation. The Cartesian geometry emplo yed restricts the present study to sectoral modes, m = +/- l. We work with l greater than or equal to 50, which guarantees that the modes do not deepl y penetrate into the solar interior and therefore experience an approximate ly uniform rotation. Potentially observable effects are predicted and devel opments of the model to aid detections are discussed.