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Supermassive black holes (SMBHs) in galactic nuclei can eject hypervelocitystars (HVSs). Using restricted three-body integrations, we study the propertiesof stars ejected by circular, binary SMBHs as a function of their mass ratios$q = M_2 / M_1$ and separations $a$, focusing on the stellar velocity andangular distributions. We find that the ejection probability is an increasingfunction of $q$ and $a$, and that the mean ejected velocity scales with $q$ and$a$ similar to previous work but with modified scaling constants. Binary SMBHstend to eject their fastest stars toward the binary orbital plane. We calculatethe ejection rates as the binary SMBHs inspiral, and find that they eject starswith velocities $v_\infty > 1000$ km/s at rates of $\sim 4 \times 10^{-2} - 2\times 10^{-1}$ yr$^{-1}$ for $q = 1$ ($\sim 10^{-4} - 10^{-3}$ yr$^{-1}$ for$q = 0.01$) over their lifetimes, and can emit a burst of HVSs with $v_\infty >3000$ km/s as they coalesce. We integrate the stellar distributions over thebinary SMBH inspiral and compare them to those produced by the "Hillsmechanism" (in which a single SMBH ejects a star after tidally separating abinary star system), and find that $N \sim 100$ HVS velocity samples with$v_\infty \gtrsim 200$ km/s are needed to confidently distinguish between abinary and single SMBH origin.

Gravitational interactions of stars with supermassive black hole binaries - II. Hypervelocity stars