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An explicit equation of the propagational angle of microwave emission betweenthe line-of-sight and the local magnetic field is newly derived. The existenceof the solution of propagational angle is clearly shown under a series oftypical parameters in solar microwave observations. It could be used todetermine the intrinsic mode and linear mode coupling in solar microwavebursts. However, a 180-degree ambiguity still exists in the direction oflongitudinal magnetic field, to produce an uncertainty of the intrinsic mode.One example is selected to check the feasibility of the method in the 2001September 25 event with a loop-like structure nearby the central meridianpassage observed by Nobeyama Radio Heliograph and Polarimeters. The calculatedangle in one footpoint (FP) varied around 90 degree in two time intervals ofthe maximum phase, which gives a direct evidence of the emission propagatingthrough a quasi-transverse region where the linear mode coupling took place,while, the angle in another FP was always smaller than 90 degrees where themode coupling did not happen. Moreover, the right-circular sense at 17 GHz wasalways observed in both two FPs during the event, which supports that thetransition frequency should be larger than 17 GHz in the first FP together withstrong magnetic field of over 2000 Gauses in photosphere, where the weaklycoupled case should happen. Moreover, there are two possibilities of theintrinsic mode in the two FPs due to the 180-degree ambiguity.

Determination of Intrinsic Mode and Linear Mode Coupling in Solar Microwave Bursts