Orbit of a Possible Planet X

The plausibility of an unseen planet in the outer solar system, and the expected orbit and mass of such a planet, have long been a topic of inquiry and debate. We calculate the long-term orbital stability of distant trans-Neptunian objects (TNOs), which allows us to expand the sample of objects that would carry dynamical information about a hypothetical unseen planet in the solar system. Using this expanded sample, we find statistically significant clustering at the ∼3σ level for TNOs with semimajor axes > 170 au in the longitude of perihelion (ϖ), but not in inclination (i), argument of perihelion (ω), or longitude of node (Ω). Since a natural explanation for clustering in ϖ is an unseen planet, we run 300 N-body simulations with the giant planets, a disk of test particles representing Kuiper Belt objects, and an additional planet with varied initial conditions for its mass, semimajor axis, eccentricity, and inclination. Based on the distribution of test particles after 1-2 Gyr, we compute relative likelihoods given the actual distribution of ϖ as a function of semimajor axis for distant TNOs on stable orbits using a significantly larger sample than previous work. We find the best-fit unseen planet parameters to have mass m_p = 4.4 ± 1.1 M_⊕, semimajor axis a_p = 290 ± 30 au, eccentricity e_p = 0.29 ± 0.13, and inclination i_p = 6 . ° 8 ± 5 . ° 0. Only 0.06% of the M. E. Brown & K. Batygin Planet Nine reference population produce probabilities within 1σ of the maximum within our quadrivariate model, indicating that our work identifies a distinct preferred region of parameter space for an unseen planet in the solar system.