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The Galactic center of the Milky-Way harbors a massive black hole (BH)orbited by a diverse population of young and old stars. A significant fractionof the youngest stars ($\sim4-7$ Myr) reside in a thin stellar disk withpuzzling properties; the disk appears to be warped, shows asymmetries, andcontains one or more clumpy structures (e.g. IRS 13). Models explaining theclumping invoked the existence of an intermediate-mass BH of $10^{3}-10^{4}$M$_{\odot}$, but no kinematic evidence for such a BH has been found. Here weuse extended $N$-body simulations and hybrid self-consistent field methodmodels to show that naturally formed residual temporal asphericity of thehosting nuclear star cluster gives rise to torques on the disk, which lead tochanges in its orientation over time, and to recurrent formation anddissolution of single spiral arm ($m=1$ modes) structures. The changingorientation leads to a flapping-like behavior of the disk and to the formationof a warped disk structure. The spiral arms may explain the over-densities inthe disk (clumping) and its observed asymmetry, without invoking the existenceof an intermediate-mass BH. The spiral arms are also important for the overalldisk evolution and can be used to constrain the structure and composition ofthe nuclear stellar cluster.

Spiral arms, warping, and clumps formation in the Galactic center young stellar disk