TY - JOUR
T1 - Effects of non-Kozai mutual inclinations on two-planet system stability through all phases of stellar evolution
AU - Veras, Dimitri
AU - Georgakarakos, Nikolaos
AU - Gänsicke, Boris T.
AU - Dobbs-Dixon, Ian
N1 - Funding Information:
We thank the referee for useful comments, which have improved the manuscript. DV gratefully acknowledges the support of the STFC via an Ernest Rutherford Fellowship (grant ST/P003850/1), and has received, along with BTG, funding from the European Research Council under the European Union’s Seventh Framework Programme (FP/2007-2013)/ERC Grant Agreement n. 320964 (WD-Tracer).
Publisher Copyright:
© 2018 The Author(s).
PY - 2018/12/1
Y1 - 2018/12/1
N2 - Previous full-lifetime simulations of single-star multi-planet systems across all phases of stellar evolution have predominately assumed coplanar or nearly coplanar orbits. Here we assess the consequences of this assumption by removing it and exploring the effect of giant branch mass loss on the stability of two-planet systems with small to moderate non-Kozai (< 40°) relative inclinations. We run nearly 104 simulations over 14 Gyr for F-star, A-star and B-star planet hosts, incorporating main-sequence stellar masses of 1.5, 2.0, 2.5, 3.0 and 5.0 solar masses, and initial planetary semimajor axis ratios that straddle their three-dimensional Hill stability limits. We find that the near-coplanar assumption can approximate well the stability frequencies and critical separations found for higher inclinations, except around strong meanmotion commensurabilities. Late instabilities - after the star has become a white dwarf - occur throughout the explored mutual inclination range. Consequently, non-Kozai mutual inclination should not be used as a predictive orbital proxy for determining whichwhite dwarfmulti-planet systems discovered by Gaia should represent high-priority follow-up targets for the detection of metal pollution and planetary debris discs.
AB - Previous full-lifetime simulations of single-star multi-planet systems across all phases of stellar evolution have predominately assumed coplanar or nearly coplanar orbits. Here we assess the consequences of this assumption by removing it and exploring the effect of giant branch mass loss on the stability of two-planet systems with small to moderate non-Kozai (< 40°) relative inclinations. We run nearly 104 simulations over 14 Gyr for F-star, A-star and B-star planet hosts, incorporating main-sequence stellar masses of 1.5, 2.0, 2.5, 3.0 and 5.0 solar masses, and initial planetary semimajor axis ratios that straddle their three-dimensional Hill stability limits. We find that the near-coplanar assumption can approximate well the stability frequencies and critical separations found for higher inclinations, except around strong meanmotion commensurabilities. Late instabilities - after the star has become a white dwarf - occur throughout the explored mutual inclination range. Consequently, non-Kozai mutual inclination should not be used as a predictive orbital proxy for determining whichwhite dwarfmulti-planet systems discovered by Gaia should represent high-priority follow-up targets for the detection of metal pollution and planetary debris discs.
KW - Asteroids: general
KW - Celestial mechanics -minor planets
KW - Methods: numerical
KW - Planets and satellites: dynamical evolution and stability
KW - Stars: AGB and post-AGB
KW - White dwarfs
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U2 - 10.1093/MNRAS/STY2409
DO - 10.1093/MNRAS/STY2409
M3 - Article
AN - SCOPUS:85060883117
VL - 481
SP - 2180
EP - 2188
JO - Monthly Notices of the Royal Astronomical Society
JF - Monthly Notices of the Royal Astronomical Society
SN - 0035-8711
IS - 2
ER -