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We discuss a model for the Milky Way obtained by fitting the observedterminal velocities with the radial acceleration relation. The resultingstellar surface density profile departs from a smooth exponential disk, havingbumps and wiggles that correspond to massive spiral arms. These features areused to estimate the term for the logarithmic density gradient in the Jeansequation, which turn out to have exactly the right location and amplitude toreconcile the apparent discrepancy between the stellar rotation curve and thatof the interstellar gas. This model also predicts a gradually decliningrotation curve outside the solar circle with slope$-1.7\;\mathrm{km}\,\mathrm{s}^{-1}\,\mathrm{kpc}^{-1}$, as subsequentlyobserved.

The Imprint of Spiral Arms on the Galactic Rotation Curve