Table 2: Parameters of the models used to study the evolution of a planetary system under the action of an outer disk. Given are a model name, the used thermodynamics (TD), isothermal (iso) or radiative (rad), the type of outer boundary condition (obc) (open or closed), the mass-ratio of the inner planet (q₁), the mass ratio or evolution of the outer planet (q₂), the figure in which the model is displayed. The displayed radiative models include heating and cooling only as the inclusion of the diffusion does not change results significantly.
Name TD obc q₁ q₂ Fig.

[10^-3] [10^-3]

h4 iso closed 1.75 3.50 9

h2 iso closed 1.75 5.9 10

h9 iso closed 2.10 7.10 11

m1 rad closed 1.75 5.9 12

k3b iso open 1.75 5.9 13

h8a iso open 2.10 5.9 $\rightarrow$ 6.9 14

m2 rad open 1.75 5.9 15

**Table 2:** Parameters of the models used to study the evolution of a planetary system under the action of an outer disk. Given are a model name, the used thermodynamics (TD), isothermal (iso) or radiative (rad), the type of outer boundary condition (obc) (open or closed), the mass-ratio of the inner planet (q₁), the mass ratio or evolution of the outer planet (q₂), the figure in which the model is displayed. The displayed radiative models include heating and cooling only as the inclusion of the diffusion does not change results significantly.
Name	TD	obc	q₁	q₂	Fig.
			[10^-3]	[10^-3]
h4	iso	closed	1.75	3.50	9
h2	iso	closed	1.75	5.9	10
h9	iso	closed	2.10	7.10	11
m1	rad	closed	1.75	5.9	12
k3b	iso	open	1.75	5.9	13
h8a	iso	open	2.10	5.9 $\rightarrow$ 6.9	14
m2	rad	open	1.75	5.9	15

Source LaTeX | All tables | In the text

	1 Introduction
	2 The system GJ 876
	3 The hydrodynamical model
	4 Model computations
	5 Interpretations
	6 Conclusion
	References