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Recent spectroscopic analysis has set an upper limit to the age of theS-stars, the ~30 B-type stars in highly eccentric orbits around thesupermassive black hole (SMBH) in the Galactic center. The inferred age (<15Myr) is in tension with the binary break-up scenario proposed to explain theirorigin. However, the new estimate is compatible with the age of the disk ofO-type stars that lies at a farther distance from the SMBH. Here we investigatea new formation scenario, assuming that both S-stars and the O-type stars wereborn in the same disk around SgrA*. We simulate encounters between binaries ofthe stellar disk and stellar black holes from a dark cusp around SgrA*. We findthat B-type binaries can be easily broken up by the encounters and their binarycomponents are kicked into highly eccentric orbits around the SMBH. Incontrast, O-type binaries are less frequently disrupted and their membersremain in low eccentricity orbits. This mechanism can reproduce 12 S-stars justby assuming that the binaries initially lie within the stellar disk as observednowadays. To reproduce all the S-stars, the original disk must have beenextended down to 0.006 pc. However in this case many B- and O-type stars remainin low eccentricity orbits below 0.03 pc, in contrast with the observations.Therefore, some other mechanism is necessary to disrupt the disk below 0.03 pc.This scenario can also explain the high eccentricity of the G-objects, if theyhave a stellar origin.

The Keplerian three-body encounter I. Insights on the origin of the S-stars and the G-objects in the Galactic center