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Recent observations suggest ongoing planet formation in the innermost parsecof the Galactic center (GC). The super-massive black hole (SMBH) might stripplanets or planetary embryos from their parent star, bringing them close enoughto be tidally disrupted. Photoevaporation by the ultraviolet field of youngstars, combined with ongoing tidal disruption, could enhance the near-infraredluminosity of such starless planets, making their detection possible even withcurrent facilities. In this paper, we investigate the chance of planet tidalcaptures by means of high-accuracy N-body simulations exploiting Mikkola'salgorithmic regularization. We consider both planets lying in the clockwise(CW) disk and planets initially bound to the S-stars. We show that tidallycaptured planets remain on orbits close to those of their parent star.Moreover, the semi-major axis of the planet orbit can be predicted by simpleanalytic assumptions in the case of prograde orbits. We find that starlessplanets that were initially bound to CW disk stars have mild eccentricities andtend to remain in the CW disk. However, we speculate that angular momentumdiffusion and scattering with other young stars in the CW disk might bringstarless planets on low-angular momentum orbits. In contrast, planets initiallybound to S-stars are captured by the SMBH on highly eccentric orbits, matchingthe orbital properties of the G1 and G2 clouds. Our predictions apply not onlyto planets but also to low-mass stars initially bound to the S-stars andtidally captured by the SMBH.

Dynamics of tidally captured planets in the Galactic Center