On radial motion of dense regions and objects in protoplanitary-like disks

TL;DR

This paper models the radial motion of dense regions in protoplanetary-like disks using a Newtonian n-body approach, providing a qualitative explanation for observed stellar motions and potential implications for spiral arm formation.

Contribution

It introduces a new modeling approach for disk dynamics that explains radial motions and explores their impact on spiral structures.

Findings

Qualitative explanation of observed radial stellar motions

Modeling of local trajectory stability in protoplanetary disks

Preliminary insights into spiral arm formation effects

Abstract

Astronomers recently discovered a non-trivial radial motion of stars within our galaxy and were able to reproduce the results using n-body numerics. I modeled a protoplanitary-like disk within a newtonian $\infty$-body problem and considered the stability of local trajectories giving a qualitative explanation to the observed radial motion. As a prospect there will be a short estimate on the impact on spiral arms.