Earth’s magnetic field is believed to be generated in the metallic outer core through a process known as the geodynamo. Direct numerical simulation (DNS) of the geodynamo has successfully reproduced many features of the Earth’s field. However, even the state-of-the-art simulations have a much higher viscosity than the Earth’s outer core. Taylor (1963) proposed a reduced model by neglecting inertia and viscous force. A modified model that partially re-introduces the inertia term back is termed the torsional wave (TW) dynamo model. Luo (2021) developed the first 3D TW dynamo model (or inviscid convective dynamo model), a branch of the fully spectral efficiently parallelized CFD code QuICC. In this study, we present new results of inviscid dynamo simulation at a higher truncation level L_{B}= 80. We observe the geostrophic flow dominates the velocity field, and the dipolar component dominates the magnetic field. The inviscid solution fundamentally differs from the viscous dynamos (with Ekman number E = 10^(-5)), which all have non-dipolar magnetic fields. Our inviscid simulation has great potential to give new insights into the geodynamo and other planetary dynamos, which current DNS can hardly achieve.