  A fraction of core-collapse supernovae (SNe) with signs of interaction with a
dense circumstellar matter are preceded by bright precursor emission. While the
precursors are likely caused by a mass ejection before core-collapse, their
mechanism to power energetic bursts, sometimes reaching $10^{48}$--$10^{49}\
{\rm erg}$ that are larger than the binding energies of red supergiant
envelopes, is still under debate. Remarkably, such a huge energy-deposition
should result in an almost complete envelope ejection and hence a strong sign
of interaction, but the observed SNe with precursors show in fact typical
properties among the interacting SNe. More generally, the observed luminosity
of $10^{40-42}\,\rm erg\,s^{-1}$ is shown to be challenging for a single SN
progenitor. To resolve these tensions, we propose a scenario where the
progenitor is in a binary system with a compact object (CO), and an outburst
from the star leads to a super-Eddington accretion onto the CO. We show that
for sufficiently short separations, outbursts with moderate initial kinetic
energies of $10^{46}$--$10^{47}$ erg can be energized by the accreting CO so
that their radiative output can be consistent with the observed precursors. We
discuss the implications of our model in relation to CO binaries detectable
with Gaia and gravitational wave detectors.
