Although bars are prevalent in disk galaxies, the precise conditions that lead to their formation remain poorly understood. In this talk, I will present results from a suite of N-body simulations that explore the onset of bar formation across galaxies with varying mass. The simulations are interpreted using swing amplification theory to clarify the mechanisms driving bar growth. I will also analyze the angular distributions of radial and azimuthal stellar velocities to identify kinematic signatures of bar-supporting orbits, and compare them with the bisymmetric model of Spekkens & Sellwood. Finally, I will discuss how bars alter rotation curves via changes in the radial pressure gradient, and compare the results with observations of barred galaxies.