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We study the 10 Myr evolution of parsec-scale stellar disks with initialmasses of $M_{\mathrm{disk}} = 1.0$ - $7.5 \times 10^4 M_\odot$ andeccentricities $e_\mathrm{init}=0.1$-$0.9$ around supermassive black holes(SMBHs). Our disk models are embedded in a spherical background potential andhave top-heavy single and binary star initial mass functions (IMF) with slopesof $0.25$-$1.7$. The systems are evolved with the N-body code$\texttt{BIFROST}$ including post-Newtonian (PN) equations of motion andsimplified stellar evolution. All disks are unstable and evolve on Myrtimescales towards similar eccentricity distributions peaking at $e_\star \sim0.3$-$0.4$. Models with high $e_\mathrm{init}$ also develop a very eccentric$(e_\star\gtrsim0.9)$ stellar population. For higher disk masses$M_\mathrm{disk} \gtrsim3 \times10^4\;\mathrm{M_\odot}$, the disk disruptiondynamics is more complex than the standard secular eccentric disk instabilitywith opposite precession directions at different disk radii - a precessiondirection instability. We present an analytical model describing this behavior.A milliparsec population of $N\sim10$-$100$ stars forms around the SMBH in allmodels. For low $e_\mathrm{init}$ stars migrate inward while for$e_\mathrm{init}\gtrsim0.6$ stars are captured by the Hills mechanism. WithoutPN, after $6$ Myr the captured stars have a sub-thermal eccentricitydistribution. We show that including PN effects prevents this thermalization bysuppressing resonant relaxation effects and cannot be ignored. The number oftidally disrupted stars is similar or larger than the number of milliparsecstars. None of the simulated models can simultaneously reproduce the kinematicand stellar population properties of the Milky Way center clockwise disk andthe S-cluster.

Evolution of eccentric stellar disks around supermassive black holes: the complex disk disruption dynamics and the milliparsec stars