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A fraction of core-collapse supernovae (SNe) with signs of interaction with adense circumstellar matter are preceded by bright precursor emission. While theprecursors are likely caused by a mass ejection before core-collapse, theirmechanism to power energetic bursts, sometimes reaching $10^{48}$--$10^{49}\{\rm erg}$ that are larger than the binding energies of red supergiantenvelopes, is still under debate. Remarkably, such a huge energy-depositionshould result in an almost complete envelope ejection and hence a strong signof interaction, but the observed SNe with precursors show in fact typicalproperties among the interacting SNe. More generally, the observed luminosityof $10^{40-42}\,\rm erg\,s^{-1}$ is shown to be challenging for a single SNprogenitor. To resolve these tensions, we propose a scenario where theprogenitor is in a binary system with a compact object (CO), and an outburstfrom the star leads to a super-Eddington accretion onto the CO. We show thatfor sufficiently short separations, outbursts with moderate initial kineticenergies of $10^{46}$--$10^{47}$ erg can be energized by the accreting CO sothat their radiative output can be consistent with the observed precursors. Wediscuss the implications of our model in relation to CO binaries detectablewith Gaia and gravitational wave detectors.

Bright Supernova Precursors by Outbursts from Massive Stars with Compact Object Companions