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Kepler's observation shows that many of the detected planets aresuper-Earths. They are inside a range of critical masses overlapping the coremasses (2-20 $M_{\bigoplus}$), which would trigger the runaway accretion anddevelop the gas giants. Thus, super-Earths/sub-Neptunes can be formed byrestraining runaway growth of gaseous envelopes. We assess the effect ofplanetary rotation in delaying the mass growth. The centrifugal force, inducedby spin, will offset a part of the gravitational force and deform the planet.Tracking the change in structure, we find that the temperature at theradiative-convective boundary (RCB) is approximate to the boundary temperature.Since rotation reduces the radiation energy densities in the convective andradiative layers, RCB will penetrate deeper. The cooling luminosity woulddecrease. Under this condition, the evolutionary timescale can exceed the disklifetime (10 Myr), and a super-Earth/sub-Neptune could be formed afterundergoing additional mass loss processes. In the dusty atmosphere, even alower angular velocity can also promote a super-Earth/sub-Neptune forming.Therefore, we conclude that rotation can slow down the planet's cooling andthen promote a super-Earth/sub-Neptune forming.

In situ formation of super-Earth/sub-Neptune driven by the planetary rotation