  Super-Earth population, as one of the representatives of exoplanets, plays an
important role in constraining the planet formation theories. According to the
prediction from core-accretion models, super-Earths should be rare because
their masses are in the range of the critical mass above which they would grow
to be gas giants by runaway gas accretion. In this work, we investigate the
effect of ohmic dissipation on the planetary thermal structure and cooling
contraction as planets accrete gas from their surrounding disks. We find that
the extra heating energy from Ohmic heating deposited into planetary envelopes
can push the planetary radiative-convective boundaries inward and prevent the
planets from cooling, and can even halt accretion. We explore parameter space
to study the dependence of cooling timescale on the input parameters of the
ohmic-dissipation model. Numerical results show that gas accretion can be
halted before runaway gas accretion and the envelope mass is only several
percent of planetary core mass for some parameter sets. Our results suggest
that ohmic dissipation is a potential mechanism to delay the gas accretion and
promote the formation of super-Earths. Future observations may help to
constrain the importance of ohmic dissipation on the super-Earth formation.
