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We use the Galaxy And Mass Assembly (GAMA) survey to measure the localUniverse mass dependent merger fraction and merger rate using galaxy pairs andthe CAS structural method, which identifies highly asymmetric merger candidategalaxies. Our goals are to determine which types of mergers produce highlyasymmetrical galaxies, and to provide a new measurement of the local galaxymajor merger rate. We examine galaxy pairs at stellar mass limits down to$M_{*} = 10^{8}M_{\odot}$ with mass ratios of $<$100:1 and line of sightvelocity differences of $\Delta V<500$ km s$^{-1}$. We find a significantincrease in mean asymmetries for projected separations less than the sum of theindividual galaxy's Petrosian 90 radii. For systems in major merger pairs withmass ratios of $<$4:1 both galaxies in the pair show a strong increase inasymmetry, while in minor merger systems (with mass ratios of $>$4:1) the lowermass companion becomes highly asymmetric, while the larger galaxy is much lessaffected. The fraction of highly asymmetric paired galaxies which have a majormerger companion is highest for the most massive galaxies and dropsprogressively with decreasing mass. We calculate that the mass dependent majormerger fraction is fairly constant at $\sim1.3-2\%$ between$10^{9.5}<M_{*}<10^{11.5} M_{\odot}$, and increases to $\sim4\%$ at lowermasses. When the observability time scales are taken into consideration, themajor merger rate is found to approximately triple over the mass range weconsider. The total co-moving volume major merger rate over the range$10^{8.0}<M_{*}<10^{11.5} M_{\odot}$ is $(1.2 \pm 0.5) \times 10^{-3}$$h^{3}_{70}$ Mpc$^{-3}$ Gyr$^{-1}$.

Galaxy And Mass Assembly (GAMA): Refining the Local Galaxy Merger Rate using Morphological Information