Improvement of the position of planet X based on the motion of nearly parabolic comets

• Published in: Astronomy letters Vol. 43; no. 2; pp. 120 - 125
• Main Authors: Medvedev, Yu. D., Vavilov, D. E., Bondarenko, Yu. S., Bulekbaev, D. A., Kunturova, N. B.
• Format: Journal Article
• Language: English
• Published: Moscow Pleiades Publishing 01.02.2017; Springer Nature B.V
• Subjects: Astronomy; Astrophysics; Astrophysics and Astroparticles; Cassini mission; Comets; Declination; Intervals; Lists; Observations and Techniques; Orbits; Physics; Physics and Astronomy; Planet detection; Planets; Solar system; planet X; ephemeris; Edgeworth–Kuiper belt; orbit; nearly parabolic comets
• DOI: 10.1134/S1063773717020037
• ISSN: 1063-7737

Based on the motion of nearly parabolic comets, we have improved the position of planet X in its orbit obtained by Batygin and Brown (2016). By assuming that some of the comets discovered to date could have close encounters with this planet, we have determined the comets with a small minimum orbit intersection distance with the planet. Five comets having hyperbolic orbits before their entry into the inner Solar system have been separated out from the general list. By assuming that at least one of them had a close encounter with the planet, we have determined the planet’s possible position. The planet’s probable ephemeris positions at the present epoch have been obtained by assuming the planet to have prograde and retrograde motions. In the case of a prograde motion, the planet is currently at a distance Δ whose value belongs to the interval Δ ∈ (1110, 1120) AU and has a right ascension α and declination δ within the intervals α ∈ (83◦, 90◦) and δ ∈ (8◦, 10◦); the true anomaly υ belongs to the interval υ ∈ (176◦, 184◦). In the case of a retrograde motion: α ∈ (48◦, 58◦), δ ∈ (−12◦, −6◦), Δ ∈ (790, 910) AU, and υ ∈ (212◦, 223◦). It should be noted that in the case of a retrograde motion of the planet, its ephemeris position obtained from the motion of comets agrees with the planet’s position obtained byHolman and Payne (2016) from highly accurate Cassini observations and is consistent with the results of Fienga et al. (2016).