Figure 14

Figure 14: The limiting rate for the evolution of the orbital periods (τ−P1 ≡ P˙∕P) of five known millisecond, accreting pulsars as a function of the Brans–Dicke parameter ω BD. The lower half of the plot corresponds to an orbital period that decreases with time (˙ P∕P < 0), whereas the upper half corresponds to an orbital period that increases with time (P˙∕P > 0). Only the area outside the two curves for each system is physically allowed [125].