Extrasolar Planet Interactions:
A Tabulation of Dynamical Characteristics

Last Update: 01 August 2011

Website maintained by Miles Timpe
 apskier@u.washington.edu

This page lists dynamical properties of published multiple planet systems. So far 2 parameters that quantify dynamical interactions have been identified: proximity to an apsidal separatrix, ε = 0 (see Barnes & Greenberg 2006a, 2006c) and proximity to the Hill stability boundary for non-resonant systems, β = 1 (see Barnes & Greenberg 2006b, 2007b). This latter boundary only applies to two-planet, non-resonant systems. The table and figures present the current dynamical properties of extra-solar planets using the best determination of their orbits from the listed reference (note that significant errors exist). Unfortunately β can only be calculated for 2-planet systems. AM stands for "Apsidal Motion", which can be Aligned libration (A), Anti-Aligned libration (AA), or Circulation (C). The "Class" identifies pairs that have undergone Tidal evolution (T), are experiencing Resonant phenomena (R), are dominated by Secular interactions (S), or the best fit is Unstable (U).

Table 1 - Dynamical Properties of Known Planetary Systems
(46 systems, 71 pairs)
SystemPairAM&epsilon&betaClassReference
47 UMa b-c C 2.64 x 10-4 - S Gregory & Fischer (2009)
c-d C 1.29 x 10-4 - S
55 Cnc e-b C 1.4 x 10-3 - T Fischer et al. (2008)
b-c AA 0.053 - S
c-f C 0.157 - S
f-d C 0.174 - S
61 Vir b-c C 0.063 - T Vogt et al. (2009)
c-d A 0.548 - S
BD-08°2823 b-c C 0.4739 1.8786 T Hébrard et al. (2009)
CoRoT-7 b-c C 0 1.18985 T Léger et al. (2009)
GJ 581 e-b C/Aa 0 - T Mayor et al. (2009)
b-c C/Aa 0 - T
c-d C 0.192 - T
GJ 876 d-c C 0 - T Butler et al. (2006)
c-b A 0.309 - R/2:1
HAT-P-13 b-c A 0.644 1.142 S Bakos et al. (2009)
HAT-P-17 b-c C 0.412 5.434 S Howard et al. (2010)
HD 9446 b-c C 0.248 1.245 S Hébrard et al. (2010)
HD 10180 b-c C 0 - T Lovis et al. (2010)
c-d C/Aa 5.66 x 10-4 - S
d-e C 4.95 x 10-4 - S
e-f C 0.033 - S
f-g C 0 - S
g-h C 0 - S
HD 11506 c-b C 0.345 1.163 S Tuomi & Kotiranta (2009)
HD 11964 c-b C 0.473 2.037 T Baines et al. (2009)
HD 12661 b-c AA 0.057 1.138 S Wright et al. (2009)
HD 17156 b-c C 0.0975 0.572 R/5:1 Short et al. (2008)
HD 37124 b-d C 0.022 - S Butler et al. (2006)
d-c A 0.148 - S
HD 38529 b-d C 0.2426 - S Wright et al. (2009)
d-c C 0.2879 - S
HD 40307 b-c C 0 - T Mayor et al. (2008)
c-d C 0 - T
HD 45364 b-c AA 0.818 0.989 R/3:2 Correia et al. (2009)
HD 47186 b-c C 0.494 6.135 S Bouchy et al. (2009)
HD 60532 b-c AA 0.0777 1.054 R/3:1 Desort et al. (2008)
HD 69830 b-c C 0.094 - T Lovis et al. (2006)
c-d C 0.040 - S
HD 73526 b-c C 0.0628 0.982 R/2:1 Saffe et al. (2005)
HD 74156 b-d C 0.002 - S Barnes et al. (2008)
d-c C 0.002 - S
HD 82943 b-c C 1.24 x 10-3 0.946 R/2:1 Butler et al. (2006)
HD 99492 b-c C 0.645 6.912 S Meschiari et al. (2010)
HD 108874 b-c AA 0.235 1.103 R/4:1 Wright et al. (2009)
HD 113538 b-c AA 1.274 1.067 S Moutou et al. (2010)
HD 128311 b-c C 0 0.970 R/2:1 Butler et al. (2006)
HD 134987 b-c AA 0.788 1.668 T Saffe et al. (2005)
HD 147018 b-c C 0.356 1.771 S Ségransan et al. (2009)
HD 155358 b-c AA 0.208 1.042 S Cochran et al. (2007)
HD 168443 b-c C 0.222 2.031 S Wright et al. (2009)
HD 169830 b-c C 0.311 1.294 S Butler et al. (2006)
HD 177830 c-b C 0.156 1.044 S Meschiari et al. (2010)
HD 181433 b-c ?c 0.016 - U Bouchy et al. (2009)
c-d ?c 1.26 x 10-6 - U
HD 183263 b-c AA 0.001 1.059 S Wright et al. (2009)
HD 187123 b-c C 0.446 15.179 T Wright et al. (2009)
HD 190360 c-b C 0.439 1.702 T Butler et al. (2006)
HD 202206 b-c C 0.096 0.883 R/5:1 Correia et al. (2005)
HD 208487 b-c C 0.171 1.263 R/7:1 Gregory (2007)
HD 217107 b-c C 0.457 9.464 T Wright et al. (2009)
HIP 14810 b-c AA 0.379 - T Wright et al. (2009)
c-d C 0.141 - S
Kepler-9 b-c C 0 1.0352 S Holman et al. (2010)
&upsilon And b-c C 0.020 - T Wright et al. (2009)
c-d A 0.114 - S
&mu Ara d-e C 0.002 - T Pepe et al. (2007)
d-b C 0.003 - R/2:1
e-b C 0.13 - S
Solar System J-S C 0.222 - S JPL
S-U C 0.094 - S
U-N C 0.032 - S

aThis pair is on the apsidal separatrix.
bThe angle of one apse is unknown
cThe published orbits are unstable.
dThe orbits are not known well enough to determine the interaction.


Figure 1. Distribution of ε values in Table 1. Most systems lie near the apsidal separatrix (ε < 0.01). Note that unstable systems are not included in this histogram.

Figure 2. Distribution of β values in Table 1. Most pairs lie near the Hill stability limit (β < 2). Note that nearly all resonantly interacting pairs have &beta < 1, which is allowed in Hill stability theory, but means if not for the resonance, these pairs would be unstable. Note that unstable systems are not included in this histogram.