In G dwarfs, the surface distribution, coverage and lifetimes of starspots deviate from solar-like patterns as the rotation rate increases. We set up a numerical platform which includes the large-scale rotational and surface flow effects, aiming to simulate evolving surface patterns over an activity cycle for up to 8 times the solar rotation and flux emergence rates. At the base of the convection zone, we assume a solar projected butterfly diagram. We then follow the rotationally distorted trajectories of rising thin flux tubes to obtain latitudes and tilt angles. Using them as source distributions, we run a surface flux transport model with solar parameters. Our model predicts surface distributions of the signed radial fields and the starspots that qualitatively agree with observations.

{"references": ["Castenmiller et al. (1986). Solar Physics 105, 207", "Isik et al. (2011) A&A 528, A135", "Isik et al. (2018). arXiv:1810.06728", "Jiang et al. (2011). A&A 528, A82", "Jiang et al. (2011). A&A 528, A83", "O'Neal et al. (2004). Astronomical Journal 128, 1802", "Pelt et al. (2010). A&A 513, A48"]}

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