Improvement of the position of planet X based on the motion of nearly parabolic comets
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 i...
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Published in | Astronomy letters Vol. 43; no. 2; pp. 120 - 125 |
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Main Authors | , , , , |
Format | Journal Article |
Language | English |
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Moscow
Pleiades Publishing
01.02.2017
Springer Nature B.V |
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Abstract | 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). |
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AbstractList | 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 Delta whose value belongs to the interval Delta (1110, 1120) AU and has a right ascension alpha and declination delta within the intervals alpha (83, 90) and delta (8, 10); the true anomaly upsilon belongs to the interval upsilon (176, 184). In the case of a retrograde motion: alpha (48, 58), delta (-12, -6), Delta (790, 910) AU, and upsilon (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). 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 [alpha] and declination δ within the intervals [alpha] (83, 90) and δ (8, 10); the true anomaly υ belongs to the interval υ (176, 184). In the case of a retrograde motion: [alpha] (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). 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). |
Author | Bulekbaev, D. A. Kunturova, N. B. Vavilov, D. E. Bondarenko, Yu. S. Medvedev, Yu. D. |
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Cites_doi | 10.1051/0004-6361/201628227 10.3847/0004-6256/151/2/22 10.1007/10651968_10 |
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References | BatyginK.BrownM. E.Astron. J.2016151222016AJ....151...22B10.3847/0004-6256/151/2/22 BondarenkoYu. S.Halley Electronic Ephemeris of Comets2016 JPL. http://ssd.jpl.nasa.gov/sbdb.cgi. Accessed 2016. FiengaA.LaskarJ.MancheH.GastineauM.Astron. Astrophys.2016587L82016A&A...587L...8F10.1051/0004-6361/201628227 K. J. Meech, O. R. Hainaut, and B. G. Marsden, Minor Bodies in the Outer Solar System, Ed. by A. Fitzsimmons et al. (Springer, 2000), p.75. BondarenkoYu.S.MedvedevYu.D.Yas’koP. P.Tr. IPA RAN201223172 The List of Split Comets. http://www.icq.eps.harvard.edu/ICQsplit.html, Accessed 2016. AbalakinV. K.AksenovE. P.GrebenikovE. A.DeminV. G.RyabovYu. A.Reference Manual on Celestial Mechanics and Astrodynamics1976865 M. Holman and M. Payne, arXiv:1604.03180v1 [astro-ph.EP] 13 Apr (2016). GulievA. S.Kinem. Fiz. Neb. Tel19941144 9626_CR7 V. K. Abalakin (9626_CR1) 1976 A. Fienga (9626_CR5) 2016; 587 9626_CR8 Yu.S. Bondarenko (9626_CR4) 2012; 23 9626_CR9 A. S. Guliev (9626_CR6) 1994; 11 K. Batygin (9626_CR2) 2016; 151 Yu. S. Bondarenko (9626_CR3) 2016 9626_CR10 |
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Snippet | 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... |
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SubjectTerms | Astronomy Astrophysics Astrophysics and Astroparticles Cassini mission Comets Declination Intervals Lists Observations and Techniques Orbits Physics Physics and Astronomy Planet detection Planets Solar system |
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Title | Improvement of the position of planet X based on the motion of nearly parabolic comets |
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