Abstract
We investigate the secular dynamics of three-body circumbinary systems under the effect of tides. We use the octupolar non-restricted approximation for the orbital interactions, general relativity corrections, the quadrupolar approximation for the spins, and the viscous linear model for tides. We derive the averaged equations of motion in a simplified vectorial formalism, which is suitable to model the long-term evolution of a wide variety of circumbinary systems in very eccentric and inclined orbits. In particular, this vectorial approach can be used to derive constraints for tidal migration, capture in Cassini states, and stellar spin–orbit misalignment. We show that circumbinary planets with initial arbitrary orbital inclination can become coplanar through a secular resonance between the precession of the orbit and the precession of the spin of one of the stars. We also show that circumbinary systems for which the pericenter of the inner orbit is initially in libration present chaotic motion for the spins and for the eccentricity of the outer orbit. Because our model is valid for the non-restricted problem, it can also be applied to any three-body hierarchical system such as star–planet–satellite systems and triple stellar systems.
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We acknowledge support from PNP-CNRS, and from CIDMA strategic Project UID/MAT/04106/2013.
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Appendices
Appendix 1: Oblate spheroid potential
The gravitational potential of an oblate body of mass \(m_i\) symmetric about its rotation axis \(\hat{\mathbf {s}}\) is given by (e.g. Goldstein 1950):
where we neglected terms in \((R_i/r)^3\). The gravity field coefficient \(J_{2,i}\) is obtained from the principal moments of inertia \(A_i= B_i\) and \(C_i\) as \(J_{2,i} = (C_i-A_i) / m_iR_i^2\). When the asymmetry in the body mass distribution results only from its rotation, \(J_{2,i}\) is given by expression (2). The main term in the above expression is responsible for the orbital motion (Eq. 4), while the contribution in \(J_{2,i}\) is responsible for a perturbation of this motion, since \( J_{2,i} (R_i/r)^2 \ll 1 \). Thus, retaining only the terms in \(J_{2,i}\), the resulting perturbing potential energy of a system composed of three oblate bodies is given by:
where we have for the planet
and for each star (\(i= 0, 1\))
We also have (Fig. 1)
where \( \delta _0= m_1/ m_{01}\) and \( \delta _1= - m_0/ m_{01}\). Since we assume that \(r_1\ll r_2\), we can write
where we neglected terms in \((r_1/ r_2)^2\), that is, we neglect terms in \(J_{2,i} (R_i/r_i)^2 (r_1/ r_2)^2\) in the potential energy. Replacing in expressions (96) and (95) we get for the planet
since \(m_0\delta _0+ m_1\delta _1= 0\), and for each star (\(i= 0,1\); \(j=1-i\))
since terms in \(m_2/ m_j(r_1/r_2)^3\) can also be neglected.
Appendix 2: Tidal potential
The tidal potential of a body of mass \(m_i\) when deformed by another body of mass \(m'\) at the position \(\mathbf {r}'\) is given by (e.g. Kaula 1964):
where we neglected terms in \((R_i/r)^4 (R_i/r')^4\). The resulting perturbing potential energy of a system composed of three bodies is given by:
where we have for the planet
and for each star (\(i= 0,1\); \(j=1-i\))
Neglecting the tidal interactions with the external body \(m_2\), i.e., neglecting terms in \(m_2/ m_j(r_1/r_2)^3\), the above potential can be simplified as
Using expression (97) we can rewrite
where we neglected terms in \((r_1/ r_2)^2\), that is, we neglect terms in \((R_2/r_2)^6 (r_1/ r_2)^2\) in the potential energy. Replacing in expression (103) we get for the planet
since \(m_0^2 \delta _0+ m_0m_1(\delta _0+ \delta _1) + m_1^2 \delta _1= 0\).
Appendix 3: Averaged quantities
For completeness, we gather here the average formulae that are used in the computation of secular equations. Let \(F(\mathbf {r},\dot{\mathbf {r}})\) be a function of a position vector \(\mathbf {r}\) and velocity \(\dot{\mathbf {r}}\), its averaged expression over the mean anomaly (M) is given by
Depending on the case, this integral is computing using the eccentric anomaly (E), or the true anomaly (v) as an intermediate variable. The basic formulae are
where \(\hat{\mathbf {k}}\) is the unit vector of the orbital angular momentum, and \(\mathbf {e}\) the Laplace–Runge–Lenz vector (Eq. 6). We have then
where \({}{\mathbf {u}}^t\) denotes the transpose of any vector \(\mathbf {u}\). This leads to
for any unit vector \(\hat{\mathbf {u}}\). In the same way,
give
The other useful formulae are
where the \(f_i(e)\) functions are given by expressions (46)–(50).
Finally, for the average over the argument of the pericenter (\(\omega \)), we can proceed in an identical manner:
which gives
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Correia, A.C.M., Boué, G. & Laskar, J. Secular and tidal evolution of circumbinary systems. Celest Mech Dyn Astr 126, 189–225 (2016). https://doi.org/10.1007/s10569-016-9709-9
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DOI: https://doi.org/10.1007/s10569-016-9709-9