“…5). Regarding the characteristics of the Kepler phase, the second term in the right-hand side of (11) can be approximated by a timedependent linear function, i.e.,z c (τ ) ≈z c1 + (z c2 −z c1 ) τ/T , wherez c1 = 2Ωv 1 sin φ 1 , z c2 = 2Ωv 2 sin φ 2 , T is the duration of the Kepler phase, and τ ∈ [0, T ] (Luo et al, 2014). Thus, Eq.…”