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Figure 1:
Planetary mass ratio, M1/M2, average orbital eccentricities,
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Figure 2: The global grid structure with gray-shaded initial surface density superimposed. Every second grid points is shown. The dots denote the location of the star and the two planets and the oval line refers to the Roche lobe of the outer planet. |
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Figure 3:
The azimuthally averaged density profile for the
relaxed configurations for three different masses of the outer planet:
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Figure 4:
Gray scale plots of the surface density ![]() ![]() ![]() |
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Figure 5: The time evolution of the semi-major axis and eccentricity for three models with different masses of the outer planet, and zero mass inner planet. |
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Figure 6: The time evolution of the periastron for three models with different masses of the outer planet. The thick dashed line is a fit corresponding to a 1 deg yr-1 shift. |
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Figure 7:
The relaxed azimuthally averaged density profile for two isothermal models with
and without considering the inner planet (solid, dotted lines),
and
two radiative models including only heating and cooling (short-dashed),
and additionally radiative diffusion (long-dashed).
The mass of the inner planet is
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Figure 8:
The relaxed azimuthally averaged temperature profile for the isothermal
(solid line) and
two radiative models including only heating and cooling (short-dashed),
and additionally radiative diffusion (long-dashed).
The mass of the inner planet is
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Figure 9:
The time evolution of the orbital elements (
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Figure 10:
The time evolution of the orbital elements (
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Figure 11:
The time evolution of the orbital elements (
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Figure 12:
The time evolution of the orbital elements (
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Figure 13:
The time evolution of the orbital elements (
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Figure 14:
The time evolution of the orbital elements (
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Figure 15:
The time evolution of the orbital elements (
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Figure 16:
Time evolution of the orbital elements (
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Figure 17:
Time evolution of the orbital eccentricities for the three-body
models with additional apsidal precession
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Figure 18: Same as Fig. 16, but for the three-body model with the following initial conditions: e1 = 0.01, e2 = 0.05, and the orbits are antialigned, with the inner planet at periapse and the outer planet at apoapse. |
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