Investigating Exoplanet Orbital Evolution Around Binary Star Systems with Mass Loss

Abstract

A planet revolving around binary star system is a familiar system. Studies of these systems are important because they provide precise knowledge of planet formation and orbit evolution. In this study, a method to determine the evolution of an exoplanet revolving around a binary star system using different rates of stellar mass loss will be introduced. Using a hierarchical triple body system, in which the outer body can be moved with the center of mass of the inner binary star as a two-body problem, the long period evolution of the exoplanet orbit is determined depending on a Hamiltonian formulation. The model is simulated by numerical integrations of the Hamiltonian equations for the system over a long time. As a conclusion, the behavior of the planet orbital elements is quite affected by the rate of the mass loss from the accompanying binary star.

Symplectic propagators for the Kepler problem with time-dependent mass

“…r with x 1 = 0, whose exact flow can be determined with the map Φ given in (3). On the other hand, and according with (23), the flow of…”

“…There are other astronomical problems that can be also modeled as (5), but, as they frequently involve some loss of mass, the corresponding Hamiltonian system depends explicitly on time. Examples are the evolution of planetary systems with time-dependent stellar loss of mass [2], evolution of exoplanets around binary star systems [23] with stellar mass loss [26], and the two-body problem with varying mass [12,24], among others [19]. The Hamilton systems to be solved are still near integrable, but non-autonomous…”

Perturbations of Zonal and Tesseral Harmonics on Frozen Orbits of Charged Satellites

“…Recall the six orbital elements (a, e, I, ω, Ω, f), namely the semimajor axis, the eccentricity, the inclination, the argument of periapsis, the longitude of the ascending node and the true anomaly respectively, and the satellite's longitude of the ascending node (ω ⊕ ) occurs inextricably linked the Earth's celestial longitude in the frame rotating with the Earth, then the Delaunay variables (l, g, h, L, G, H) can be read as; Delhaise & Morbidelli (1993) and Rahoma (2014Rahoma ( , 2016:…”