Fig. 2
Temporal variation of the mid-eclipse times of NN Ser as predicted by our best-fitting dynamical two-planet model of Table 2 relative to the underlying linear ephemeris of the binary and folded over the orbital period of the outer planet. The first two orbits, covering a time interval of 30 yr (black curves), and the next 29 orbits (30–500 yr, red curves) are displayed.
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