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Table 1.

Value of the different terms of the stability criterion u for different hydro simulations with identical initial conditions except for the masses of the co-orbitals, given in the first two columns.

m1 m2 R1ζ R2ζ 2u CΓ K1 K2

[M] [M] [yr−1] [yr−1] [yr−1] [yr−1] [yr−1] [yr−1] [yr−1] [rad yr−1]
3.0 5.0 3.9e−6 −2.0e−5 1.4e−5 1.3e−5 2.2e−5 4.2e−6 3.6e−5 5.9e−6 6.5e−2 −1 2
3.0 3.0 5.1e−6 −3.1e−5 7.7e−6 6.4e−6 −1.8e−5 4.1e−6 −2.6e−5 −4.1e−6 2.2e−2 −3 −0.9
5.0 3.0 1.1e−5 −7.4e−5 7.4e−6 5.4e−6 −5.8e−5 7.3e−6 −1.0e−4 −1.9e−5 −1.9e−2 −5 −3

3.0 15.0 5.4e−7 −6.2e−5 5.7e−5 5.1e−5 2.0e−4 1.7e−6 2.5e−4 3.2e−5 1.7e−1 −1e1 1e1
6.0 12.0 5.8e−6 −2.3e−5 3.4e−5 3.6e−5 1.9e−4 4.0e−6 2.5e−4 4.1e−5 1.1e−1 −0.5 6
10.0 10.0 1.6e−5 1.8e−4 2.7e−5 2.5e−5 −2.6e−4 6.8e−6 −9.1e−6 −2.8e−6 4.4e−2 6 −5
12.0 6.0 3.1e−5 3.1e−5 1.4e−5 9.3e−6 −2.2e−4 2.4e−5 −1.1e−4 −1.8e−5 −5.5e−2 2 −5
15.0 3.0 4.8e−5 −2.6e−4 7.1e−6 1.9e−6 −8.2e−5 1.8e−5 −2.7e−4 −4.5e−5 −1.4e−1 −1e1 −4

1.0 333 8.5e−8 2.3e−4 −3.2e−4 2.1e−5 1.7e−5 −1.3e−6 −4.9e−5 4.6e−6 −1.1e−3 5 1e2
333 1.0 2.1e−5 1.7e−5 −1.6e−6 −1.2e−7 2.9e−4 −2.8e−4 4.3e−5 2.1e−6 −9.9e−3 1e2 −3

Notes. The upper block shows the three models with low-mass planets which do not alter the surface density profile. In the second block, the planets are more massive and perturb the disc by creating a shallow gap around their orbits. In the two models of the last block, we used a full gap-opening planet as one of the co-orbitals in order to eliminate the co-rotation torque on the low-mass one.

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