Mass Transport and Turbulence in Gravitationally Unstable Disk Galaxies. I: The Case of Pure Self-Gravity

摘要: The role of gravitational instability-driven turbulence in determining the structure and evolution disk galaxies, extent to which gravity rather than feedback can explain galaxy properties, remains an open question. To address it, we present high resolution adaptive mesh refinement simulations Milky Way-like isolated including realistic heating cooling rates a physically motivated prescription for star formation, but no form formation feedback. After initial transient, our galaxies reach state fully-nonlinear instability. In this state, drives radial inflow. Despite lack feedback, gas models shows substantial turbulent velocity dispersions, indicating that instability alone may be able power dispersions observed nearby on 100 pc scales. Moreover, rate mass transport produced by approaches $\sim 1$ $M_\odot$ yr$^{-1}$ conditions, sufficient fully fuel inner disks galaxies. companion paper add models, use comparison between two cases understand what properties depend sensitively understood as product alone. All code, simulation data model are publicly available.