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We consider fallback accretion after an ultra-stripped supernova (USSN) thataccompanies formation of a binary neutron star (BNS) or a neutron star-blackhole binary (NS-BH). The fallback matter initially accretes directly to thenascent NS, while it starts to accrete to the circumbinary disk, typically$0.1\mbox{-}1\, \mathrm{day}$ after the onset of the USSN explosion. Thecircumbinary disk mass further accretes, forming mini disks around each compactobject, with a super-Eddington rate up to a few years. We show that such asystem constitutes a binary ultraluminous X-ray source (ULX), and a fraction ofthe X rays can emerge through the USSN ejecta. We encourage follow-upobservations of USSNe within $\lesssim 100\,\rm Mpc$ and $\sim100\mbox{-}1,000\,\mathrm{day}$ after the explosion using Chandra, XMM Newtonand NuSTAR, which could detect the X-ray counterpart with time variationsrepresenting the properties of the nascent compact binary, e.g., the orbitalmotion of the binary, the spin of the NS, and/or the quasiperiodic oscillationof the mini disks.

X-raying the Birth of Binary Neutron Stars and Neutron Star-Black Hole Binaries