A simple scaling for the minimum instability time-scale of two widely spaced planets

Dimitri Veras, Alexander Mustill

Forskningsoutput: TidskriftsbidragArtikel i vetenskaplig tidskriftPeer review

25 Citeringar (SciVal)

Sammanfattning

Long-term instability in multiplanet exosystems is a crucial consideration when confirming putative candidates, analysing exoplanet populations, constraining the age of exosystems and identifying the sources of white dwarf pollution. Two planets that are Hill stable are separated by a wide-enough distance to ensure that they will never collide. However, Hill-stable planetary systems may eventually manifest Lagrange instability when the outer planet escapes or the inner planet collides with the star. We show empirically that for two nearly coplanar Hill-stable planets with eccentricities less than about 0.3, instability can manifest itself only after a time corresponding to x initial orbits of the inner planet, where log10 x ~ 5.2[μ/(MJupiter/M☉)]-0.18 and μ is the planet-star mass ratio. This relation applies to any type of equal-mass secondaries, and suggests that two low-eccentricity Hill-stable terrestrial-mass or smaller mass planets should be Lagrange stable throughout the main-sequence lifetime of any white dwarf progenitor. However, Hill-stable giant planets are not guaranteed to be Lagrange stable, particularly within a few tens of per cent beyond the critical Hill separation. Our scaling represents a useful `rule of thumb' for planetary population syntheses or individual systems for which performing detailed long-term integrations is unfeasible.
Originalspråkengelska
Sidor (från-till)L11-L15
TidskriftMonthly Notices of the Royal Astronomical Society: Letters
Volym434
Utgåva1
DOI
StatusPublished - 2013
Externt publiceradJa

Ämnesklassifikation (UKÄ)

  • Astronomi, astrofysik och kosmologi
  • Fysik

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