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In this paper, we investigate the link between the hypervelocity stars (HVSs)discovered in the Galactic halo and the S-stars moving in the Galactic center(GC), under the hypothesis that they are both the products of the tidal breakupof the same population of stellar binaries by the central massive black hole(MBH). By adopting several hypothetical models for binaries to be injected intothe vicinity of the MBH and doing numerical simulations, we realize the tidalbreakup processes of the binaries and their follow-up evolution. We find thatmany statistical properties of the detected HVSs and S-stars can be reproducedunder some binary injecting models, and their number ratio can be reproduced ifthe stellar initial mass function is top-heavy (e.g., with slope ~-1.6). Thetotal number of the captured companions is ~50 that have masses in the range~3-7Msun and semimajor axes <~4000 AU and survive to the present within theirmain-sequence lifetime. The innermost one is expected to have a semimajor axis~300-1500 AU and a pericenter distance ~10-200 AU, with a significantprobability of being closer to the MBH than S2. Future detection of such acloser star would offer an important test to general relativity. The majorityof the surviving ejected companions of the S-stars are expected to be locatedat Galactocentric distances <~20 kpc, and have heliocentric radial velocities~-500-1500 km/s and proper motions up to ~5-20 mas/yr. Future detection ofthese HVSs may provide evidence for the tidal-breakup formation mechanism ofthe S-stars.

astrophysical journal/the astrophysical journal

S-stars in the Galactic center and hypervelocity stars in the Galactic  halo: two faces of the tidal breakup of stellar binaries by the central  massive black hole?