Type I migration can be defeated for super-Earths in inviscid disks. Shown here are the orbital radii vs. time of planets in three of our simulations: a single 10 M_⊕ planet in a gas-rich (Σ₀ = 8.5 × 10³ g cm⁻²) viscous (α = 10⁻³) disk (blue, model 1); a single planet of the same mass in a gas-rich inviscid (α = 0) disk (black, model 2); and two such planets in a gas-rich inviscid disk (red+magenta, model 3). The blue dashed line is the theoretically expected trajectory from Type I migration (the integral of Equation (13) with C = 2).