Neptune's capture of its moon Triton in a binary–planet gravitational encounter

Triton is Neptune's principal satellite and is by far the largest retrograde satellite in the Solar System (its mass is ∼40 per cent greater than that of Pluto). Its inclined and circular orbit lies between a group of small inner prograde satellites and a number of exterior irregular satellites with both prograde and retrograde orbits. This unusual configuration has led to the belief that Triton originally orbited the Sun before being captured in orbit around Neptune. Existing models for its capture, however, all have significant bottlenecks that make their effectiveness doubtful. Here we report that a three-body gravitational encounter between a binary system (of ∼103-kilometre-sized bodies) and Neptune is a far more likely explanation for Triton's capture. Our model predicts that Triton was once a member of a binary with a range of plausible characteristics, including ones similar to the Pluto–Charon pair.

[1]  Re'em Sari,et al.  Formation of Kuiper-belt binaries by dynamical friction and three-body encounters , 2002, Nature.

[2]  Harold F. Levison,et al.  Planetary migration in a planetesimal disk: why did Neptune stop at 30 AU? , 2004 .

[3]  K. Noll,et al.  Detection of Six Trans-Neptunian Binaries with NICMOS: A High Fraction of Binaries in the Cold Classical Disk , 2005, astro-ph/0510130.

[4]  Daniel D. Durda,et al.  Asteroids Do Have Satellites , 2002 .

[5]  Dale P. Cruikshank,et al.  Neptune and Triton , 1995 .

[6]  J. Lissauer,et al.  Formation of the Neptune system , 1995 .

[7]  T. McCord Dynamical evolution of the Neptunian system. , 1966 .

[8]  Derek C. Richardson,et al.  The formation of asteroid satellites in large impacts: Results from numerical simulations , 2004 .

[9]  Steven Soter,et al.  Q in the solar system , 1966 .

[10]  Douglas C. Heggie,et al.  Binary evolution in stellar dynamics , 1975 .

[11]  B. Gladman,et al.  CONSTRAINTS ON THE ORBITAL EVOLUTION OF TRITON , 2005, astro-ph/0505235.

[12]  Planet formation by coagulation: A focus on Uranus and Neptune , 2004, astro-ph/0405215.

[13]  W. McKinnon,et al.  Gas Drag and the Orbital Evolution of a Captured Triton , 1995 .

[14]  J. Burns,et al.  Gas drag in primordial circumplanetary envelopes: A mechanism for satellite capture , 1979 .

[15]  Joseph A. Burns,et al.  Orbital stability zones about asteroids: II. The destabilizing effects of eccentric orbits and of solar radiation , 1992 .

[16]  Orbital Evolution of Planets Embedded in a Planetesimal Disk , 1999, astro-ph/9902370.

[17]  K. S. Noll,et al.  Detection of Six Transneptunian Binaries with NICMOS: A High Fraction of Binaries in the Cold Classical Disk , 2005 .

[18]  W. McKinnon,et al.  On the origin of Triton and Pluto , 1984, Nature.

[19]  S. Cornell,et al.  A Giant Impact Origin of Pluto-Charon , 2005 .

[20]  J. Hills Computer simulations of encounters between massive black holes and binaries , 1991 .

[21]  K. H. Tsui Satellite capture in a four-body system , 2002 .

[22]  Alessandro Morbidelli,et al.  Scenarios for the Origin of the Orbits of the Trans-Neptunian Objects 2000 CR105 and 2003 VB12 (Sedna) , 2004, astro-ph/0403358.

[23]  D. Banfield,et al.  Neptune's Story , 1989, Science.

[24]  D. Campbell,et al.  Binary Asteroids in the Near-Earth Object Population , 2002, Science.

[25]  Formation of Kuiper-belt binaries through multiple chaotic scattering encounters with low-mass intruders , 2005, astro-ph/0504060.

[26]  S. Weidenschilling On the Origin of Binary Transneptunian Objects , 2002 .

[27]  Erik Asphaug,et al.  Structure of Comet Shoemaker-Levy 9 Inferred from the Physics of Tidal Breakup , 1996 .