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We explore the scaling between the size of star-forming clumps and rotationalsupport in massively star-forming galactic disks. The analysis relies onsimulations of a clumpy galaxy at $z=2$ and the observed DYNAMO sample of rareclumpy analogs at $z\approx0.1$ to test a predictive clump size scalingproposed by \citet{Fisher2017ApJ...839L...5F} in the context of the ViolentDisk Instability (VDI) theory. We here determine the clump sizes using arecently presented 2-point estimator, which is robust against resolution/noiseeffects, hierarchical clump substructure, clump-clump overlap and othergalactic substructure. After verifying Fisher's clump scaling relation for theDYNAMO observations, we explore whether this relation remains characteristic ofthe VDI theory, even if realistic physical processes, such as local asymetriesand stellar feedback, are included in the model. To this end, we rely onhydrodynamic zoom-simulations of a Milky Way-mass galaxy with four differentfeedback prescriptions. We find that, during its marginally stable epoch at$z=2$, this mock galaxy falls on the clump scaling relation, although itsposition on this relation depends on the feedback model. This finding impliesthat Toomre-like stability considerations approximately apply to large($\sim\rm kpc$) instabilities in marginally stable turbulent disks,irrespective of the feedback model, but also emphasizes that the global clumpdistribution of a turbulent disk depends strongly on feedback.

Size-scaling of clump instabilities in turbulent, feedback regulated disks