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AMD-Stability in the Presence of First-Order Mean Motion Resonances

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AMD-Stability in the Presence of First-Order Mean Motion Resonances A&A 607, A35 (2017) Astronomy DOI: 10.1051/0004-6361/201731196 & c ESO 2017 Astrophysics AMD-stability in the presence of first-order mean motion resonances A. C. Petit, J. Laskar, and G. Boué ASD/IMCCE, CNRS-UMR 8028, Observatoire de Paris, PSL Research University, UPMC, 77 avenue Denfert-Rochereau, 75014 Paris, France e-mail: [email protected] Received 18 May 2017 / Accepted 10 July 2017 ABSTRACT The angular momentum deficit (AMD)-stability criterion allows to discriminate between a priori stable planetary systems and systems for which the stability is not granted and needs further investigations. AMD-stability is based on the conservation of the AMD in the averaged system at all orders of averaging. While the AMD criterion is rigorous, the conservation of the AMD is only granted in absence of mean-motion resonances (MMR). Here we extend the AMD-stability criterion to take into account mean-motion reso- nances, and more specifically the overlap of first-order MMR. If the MMR islands overlap, the system will experience generalized chaos leading to instability. The Hamiltonian of two massive planets on coplanar quasi-circular orbits can be reduced to an integrable one degree of freedom problem for period ratios close to a first-order MMR. We use the reduced Hamiltonian to derive a new overlap criterion for first-order MMR. This stability criterion unifies the previous criteria proposed in the literature and admits the criteria obtained for initially circular and eccentric orbits as limit cases. We then improve the definition of AMD-stability to take into account the short term chaos generated by MMR overlap. We analyze the outcome of this improved definition of AMD-stability on selected multi-planet systems from the Extrasolar Planets Encyclopædia. Key words. celestial mechanics – planets and satellites: general – planets and satellites: dynamical evolution and stability – planets and satellites: atmospheres 1. Introduction In studies of planetary systems architecture, a minimal distance based on the Hill radius (Marchal & Bozis 1982) The angular momentum deficit (AMD)-stability criterion is often used as a criterion of stability (Gladman 1993; (Laskar 2000; Laskar & Petit 2017) allows to discriminate be- Chambers et al. 1996; Smith & Lissauer 2009; Pu & Wu 2015). tween a-priori stable planetary systems and systems needing an However, Deck et al.(2013) suggested that stability criteria in-depth dynamical analysis to ensure their stability. The AMD- based on the MMR overlap are more accurate in characterizing stability is based on the conservation of the angular momentum the instability of the three-body planetary problem. deficit (AMD, Laskar 1997) in the secular system at all orders Based on the considerations of Chirikov(1979) for the over- of averaging (Laskar 2000; Laskar & Petit 2017). Indeed, the lap of resonant islands, Wisdom(1980) proposed a criterion of conservation of the AMD fixes an upper bound to the eccen- stability for the first-order MMR overlap in the context of the re- tricities. Since the semi-major axes are constant in the secular stricted circular three-body problem. This stability criterion de- approximation, a low enough AMD forbids collisions between fines a minimal distance between the orbits such that the first- planets. The AMD-stability criterion has been used to classify order MMR overlap with one another. For orbits closer than this planetary systems based on the stability of their secular dynam- minimal distance, the MMR overlapping induces chaotic behav- ics (Laskar & Petit 2017). ior eventually leading to the instability of the system. However, while the analytical criterion developed in Wisdom showed that the width of the chaotic region (Laskar & Petit 2017) does not depend on series expansions for in the circular restricted problem is proportional to the ra- small masses or spacing between the orbits, the secular hypoth- tio of the planet mass to the star mass to the power 2=7. esis does not hold for systems experiencing mean motion reso- Duncan et al.(1989) confirmed numerically that orbits closer nances (MMR). Although a system with planets in MMR can be than the Wisdom’s MMR overlap condition were indeed unsta- dynamically stable, chaotic behavior may result from the over- ble. More recently, another stability criterion was proposed by lap of adjacent MMR, leading to a possible increase of the AMD Mustill & Wyatt(2012) to take into account the planet’s eccen- and eventually to close encounters, collisions or ejections. For tricity. Deck et al.(2013) improved the two previous criteria by systems with small orbital separations, averaging over the mean developing the resonant Hamiltonian for two massive, coplanar, anomalies is thus impossible due to the contribution of the first- low-eccentricity planets and Ramos et al.(2015) proposed a cri- order MMR terms. For example, two planets in circular orbits terion of stability taking into account the second-order MMR in very close to each other are AMD-stable, however the dynamics the restricted three-body problem. of this system cannot be approximated by the secular dynamics. While Deck’s criteria are in good agreement with numer- We thus need to modify the notion of AMD-stability in order to ical simulations (Deck et al. 2013) and can be applied to the take into account those configurations. three-body planetary problem, the case of circular orbits is still Article published by EDP Sciences A35, page 1 of 17 A&A 607, A35 (2017) treated separately from the case of eccentric orbits. Indeed, the which is simply the sum of the two planets Keplerian angular minimal distance imposed by the eccentric MMR overlap sta- momentum. Gˆ is a first integral of the system. bility criterion vanishes with eccentricities and therefore can- Following Laskar(1991), we express the Hamiltonian in not be applied to systems with small eccentricities. In this case, terms of the Poincaré coordinates Mustill & Wyatt(2012) and Deck et al.(2013) use the criterion ˆ ˆ developed for circular orbits. A unified stability criterion for H = Kˆ + "H1(Λˆ i; xˆi; xˆ¯i) first-order MMR overlap had yet to be proposed. 2 2 3 2 X µ m X Y ¯ In this paper, we propose in Sect.2 a new derivation of the i ˆ li ¯li ikiλi = − + " Cl;l¯;k(Λ) xˆ xˆ e ; (6) 2Λˆ 2 i i MMR overlap criterion based on the development of the three- i=1 i l;l¯2N2 i=1 body Hamiltonian by Delisle et al.(2012). We show in Sect.3 k2Z2 how to obtain a unified criterion of stability working for both initially circular and eccentric orbits. In Sect.4, we then use the where µ = Gm0 and for i = 1; 2, defined stability criterion to limit the region where the dynamics p Λˆ = m µa can be considered to be secular and adapt the notion of AMD- i i i q stability thanks to the new limit of the secular dynamics. Finally Gˆ = Λˆ 1 − e2 we study in Sect.5 how the modification of the AMD-stability i i i definition affects the classification proposed in Laskar & Petit Cˆi = Λˆ i − Gˆi (2017). q −i$i xˆi = Cˆie 2. The resonant Hamiltonian λi = Mi + $i: The problem of two planets close to a first-order MMR on nearly Here, Mi corresponds to the mean anomaly, $i to the lon- circular and coplanar orbits can be reduced to a one-degree- gitude of the pericenter, ai to the semi-major axis and ei to of-freedom system through a sequence of canonical transfor- the eccentricity of the Keplerian orbit of the planet i. Gˆi is mations (Wisdom 1986; Henrard et al. 1986; Delisle et al. 2012, the Keplerian angular momentum of planet i. We use the set 2014). We follow here the reduction of the Hamiltonian used in of symplectic coordinates of the problem (Λˆ i; λi; Cˆi; −$i), or Delisle et al.(2012, 2014). the canonically associated variables (Λˆ i; λi; xˆi; −ixˆ¯i). The coef- ˆ ficients Cl;l¯;k depend on Λ and the masses of the bodies. They are 2.1. Averaged Hamiltonian in the vicinity linear combinations of Laplace coefficients (Laskar & Robutel of a resonance 1995). As a consequence of angular momentum conservation, the d’Alembert rule gives a relation on the indices of the non- Let us consider two planets of masses m1 and m2 orbiting a star zero Cl;l¯;k coefficients of mass m0 in the plane. We denote the positions of the plan- 2 ets, ui, and the associated canonical momenta in the heliocentric X − ¯ frame, u˜ i. The Hamiltonian of the system is (Laskar & Robutel ki li + li = 0: (7) 1995) i=1 2 0 2 1 We study here a system with periods close to the first-order X 1 ku˜ k m m ∗ ˆ B i 0 i C MMR p : p + 1 with p 2 N . For periods close to this con- H = B − G C @2 mi ui A 2 3 ˆ 3 i=1 figuration, we have −pn1 + (p + 1)n2 ' 0, where ni = µ mi =Λi 1 ku˜ + u˜ k2 m m is the Keplerian mean motion of the planet i. + 1 2 − G 1 2 (1) 2 m0 ∆12 2.1.1. Averaging over non-resonant mean-motions where ∆12 = ku1 − u2k, and G is the constant of gravitation. Hˆ can be decomposed into a Keplerian part Kˆ describing the Due to the p : p + 1 resonance, we cannot average on both motion of the planets if they had no masses and a perturbation mean anomalies independently. Therefore, there is no conser- ˆ part "Hˆ due to the influence of massive planets, vation of Λi as in the secular problem.
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