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Recently, we have performed research on the subject of the cosmologicalconstant problem. The scenario is based on two postulates for inflationarytheory: one is that inflaton $\phi$ can interact with radiation (relativisticparticles); the other is that radiation will be created continuously during andafter the epoch of inflation. According to these postulates and from a"macroscopic perspective", we discover that radiation can be viewed as aproduct of the interaction between $\dot{\phi}$ and some "effective kineticfrictional force" that exists in inflaton dynamics. Deducing and surmising from"effective friction", we obtain conclusions of two special types of expandinguniverse: A Type I universe will finally enter an expanding course after aspecial time $t_{*}$ with uniformly rolling $\dot{\phi}(t_{*})$ due to thebalance between $V^{'}(\phi(t))$, 3H(t)\dot{\phi}(t_{*}) and the "effectivekinetic frictional force". In this result, the expanding course will seeparticles created continuously. Additionally, for a Type II universe, $\phi$will be at rest after $t_{r}$ inside a region named the "stagnant zone" that isformed by the "maximum effective static frictional force". Consistent withthis, inflaton potential will survive as a relic $V(\phi(t_{r}))$, playing therole of the effective cosmological constant $\Lambda$ .

The creation of radiation and the relic of inflaton potential