Table 7: Time development of orbital variability near stability boundary for P-type orbits.
$M_{\rm B} / M_{\rm A}$ $R_{\rm B}/R_{\rm A}$ 1 K 5 K 10 K 20 K 30 K 40 K
    [%] [%] [%] [%] [%] [%]

0.10		 1.95 4.16005 4.11282 4.08047 4.05153 4.03336 4.04495
0.15 2.05 4.19949 4.19578 4.19493 4.19248 4.19492 4.19569
0.33 2.25 4.81418 4.70511 4.79329 4.79473 4.79914 ...
0.50 2.35 4.99639 4.99501 4.99456 4.99473 4.99439 ...
0.60 2.40 4.98571 4.98039 4.98185 4.98188 4.98139 ...
0.90 2.45 4.99734 4.99471 4.99501 4.99483 4.98991 ...

Note: Simulations were performed for giant planets with $M_{\rm G}$ = 1  $M_{\rm Jup}$.

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Article Contents
1 Introduction
2 Method and code testing
3 Initial conditions and stability criteria
4 Case studies
5 Binary systems with observed giant planets
6 Conclusions
References
List of tables
List of figures