BH separation in kpc (top), black hole accretion rate (BHAR) in M_⊙ yr^-1 (second row), gas mass in M_⊙ within spheres up to 1 kpc in radius (third row), and SFR in M_⊙ yr^-1 within the same spheres (bottom row) vs. time for a 4:1 merger with gasoline (left) and ramses (right). For each simulation, we show quantities for the primary galaxy/BH on the left, and the secondary galaxy/BH on the right. We show gas masses and SFRs within radii of 200 pc to 1 kpc, in increments of 200 pc. Quantities are smoothed on 10 Myr timescales. Note that time-axes differ by ~20% (see Sect. 3.2.1). Vertical dotted lines mark local minima in the separation between the two black holes in all panels. The gasoline and ramses simulations show qualitatively similar results: enhanced accretion and star formation rates at the second pericenter, and especially at the third pericenter/coalescence.