Volume 530, June 2011
|Number of page(s)||11|
|Section||Planets and planetary systems|
|Published online||05 May 2011|
Last giant impact on the Neptunian system
Constraints on oligarchic masses in the trans-Saturnian region
Instituto Argentino de Radioastronomía (IAR-CONICET),
C.C. No 5,
2 Facultad de Ciencias Astronómicas y Geofísicas, Universidad Nacional de La Plata, Argentina
3 Departamento de Astronomía, Universidad de Chile, Casilla 36-D, Santiago, Chile
Received: 7 December 2010
Accepted: 4 February 2011
Context. Current models of the formation of ice giants attempt to account for the formation of Uranus and Neptune within the protoplanetary disk lifetime. Many of these models calculate the formation of Uranus and Neptune in a disk that may be several times the minimum mass solar nebula model (MMSN). Modern core accretion theories assume the formation of the ice giants either in situ, or between ~10–20 AU in the framework of the Nice model. However, at present, none of these models account for the spin properties of the ice giants.
Aims. Stochastic impacts by large bodies are, at present, the usually accepted mechanisms able to account for the obliquity of the ice giants. We attempt to set constraints on giant impacts as the cause of Neptune’s current obliquity in the framework of modern theories. We also use the present orbital properties of the Neptunian irregular satellites (with the exception of Triton) to set constraints on the scenario of giant impacts at the end of Neptune formation.
Methods. Since stochastic collisions among embryos are assumed to occur beyond oligarchy, we model the angular momentum transfer to proto-Neptune and the impulse transfer to its irregular satellites by the last stochastic collision (GC) between the protoplanet and an oligarchic mass at the end of Neptune’s formation. We assume a minimum oligarchic mass mi of 1 m⊕.
Results. From angular momentum considerations, we obtain that an oligarchic mass mi ~ 1 m⊕ ≤ mi ≤ 4 m⊕ would be required at the GC to reproduce the present rotational properties of Neptune. An impact with mi > 4 m⊕ is not possible, unless the impact parameter of the collision were very small. This result is invariant either Neptune had formed in situ or between 10–20 AU and does not depend on the occurrence of the GC after or during the possible migration of the planet. From impulse considerations, we find that an oligarchic mass mi ~ 1 m⊕ ≤ mi ≤ 1.4 m⊕ at the GC is required to keep or capture the present population of irregular satellites. If mi had been higher, the present Neptunian irregular satellites had to be formed or captured after the end of stochastic impacts.
Conclusions. The upper bounds on the oligarchic masses (4 m⊕ from the obliquity of Neptune and 1.4 m⊕ from the Neptunian irregular satellites) are independent of unknown parameters, such as the mass and distribution of the planetesimals, the location at which Uranus and Neptune were formed, the Solar Nebula initial surface mass density, and the growth regime. If stochastic impacts had occurred, these results should be understood as upper constraints on the oligarchic masses in the trans-Saturnian region at the end of ice planet formation and may be used to set constraints on planetary formation scenarios.
Key words: planets and satellites: general / planets and satellites: formation
© ESO, 2011
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