A simple formula for the third integral of motion of disk-crossing stars in the Galaxy

Abstract

We present an analytical simple formula for an approximated third integral of motion associated with nearly equatorial orbits in the Galaxy: $I_3=Z{\Sigma }_I^{1/3}$, where $Z(R)$ is the vertical amplitude of the orbit at galactocentric distance $R$ and ${\Sigma }_I(R)$ is the integrated dynamical surface mass density of the disk, a quantity which has recently become measurable. We also suggest that this relation is valid for disk-crossing orbits in a wide variety of axially symmetric galactic models, which range from razor-thin disks to disks with non-negligible thickness, whether or not the system includes bulges and halos. We apply our formalism to a Miyamoto-Nagai model and to a realistic model for the Milky Way. In both cases, the results provide fits for the shape of nearly equatorial orbits which are better than the corresponding curves obtained by the usual adiabatic approximation when the orbits have vertical amplitudes comparable to the disk's scale height. We also discuss the role of this approximate third integral of motion in modified theories of gravity.

Version accepted for publication in ApJ

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Cited by in corpus (7)

• Integrability of motion around galactic razor-thin disks
• Vertical stability of circular orbits in relativistic razor-thin disks
• Envelopes and vertical amplitudes of disk-crossing orbits
• Envelopes for orbits around axially symmetric sources with spheroidal shape
• Chaotic dynamics of pulsating spheres orbiting black holes
• Chaotic orbital dynamics of pulsating stars around black holes surrounded by dark matter halos
• Post-Newtonian Hamiltonian dynamics: applications to stationary spacetimes and statistical mechanics