Scale-free equilibria of self-gravitating gaseous disks with flat rotation curves

Abstract

We introduce exact analytical solutions of the steady-state hydrodynamic equations of scale-free, self-gravitating gaseous disks with flat rotation curves. We express the velocity field in terms of a stream function and obtain a third-order ordinary differential equation (ODE) for the angular part of the stream function. We present the closed-form solutions of the obtained ODE and construct hydrodynamical counterparts of the power-law and elliptic disks, for which self-consistent stellar dynamical models are known. We show that the kinematics of the Large Magellanic Cloud can well be explained by our findings for scale-free elliptic disks.

AAS preprint format, 21 pages, 8 figures, accepted for publication in The Astrophysical Journal

References in corpus (5)

• Magellanic Cloud Structure from Near-IR Surveys I: The Viewing Angles of the LMC
• Magellanic Cloud Structure from Near-IR Surveys II: Star Count Maps and the Intrinsic Elongation of the LMC
• Singular Isothermal Disks: II. Nonaxisymmetric Bifurcations and Equilibria
• Self-Similar Equilibria of Self-Gravitating, Magnetized, Rotating, Isothermal Systems
• The curvature condition for self-consistent scale-free galaxies

Cited by in corpus (2)

• The Case Against Dark Matter and Modified Gravity: Flat Rotation Curves Are a Rigorous Requirement in Rotating Self-Gravitating Newtonian Gaseous Disks
• Unstable modes of non-axisymmetric gaseous discs