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The Dynamic Model of the Solar System in the Planet Ephemerides EPM

E. V. Pitjeva, D. A. Pavlov, N. P. Pitjev

Transactions of IAA RAS, issue 51, 82—92 (2019)

Keywords: celestial mechanics, planet ephemerides, radar observations, asteroids, TNO, effects of General Relativity

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Abstract

Currently, the accuracy of determining coordinates in the EPM ephemeris is several meters for the inner planets and 10-20 meters for Jupiter and Saturn. The need to build more accurate ephemeris of planets requires improving the dynamic model of the solar system. When constructing the ephemeris of the bodies of the solar system, perturbations from the Sun, planets, and the Moon, as well as the main relativistic effects are usually taken into account. The perturbations of the next order of smallness , which also affect the motion of the planets, are also considered in the paper. Such perturbations are the the following: the attraction from the Main asteroid belt, Kuiper belt, Jupiter’s trojans, as well oblateness of the Sun and the relativistic Lense-Thirring effect. In addition, the influence of all these perturbations on the motion of the solar system planets is estimated and the regions in the solar system where the influence of these perturbations is most pronounced are given.

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E. V. Pitjeva, D. A. Pavlov, N. P. Pitjev. The Dynamic Model of the Solar System in the Planet Ephemerides EPM // Transactions of IAA RAS. — 2019. — Issue 51. — P. 82—92.

@article{pitjeva2019,
  abstract = {Currently, the accuracy of determining coordinates in the EPM ephemeris is several meters for the inner planets and 10-20 meters for Jupiter and Saturn. The need to build more accurate ephemeris of planets requires improving the dynamic model of the solar system. When constructing the ephemeris of the bodies of the solar system, perturbations from the Sun, planets, and the Moon, as well as the main relativistic effects are usually taken into account. The perturbations of the next order of smallness , which also affect the motion of the planets, are also considered in the paper. Such perturbations are the the following: the attraction from the Main asteroid belt, Kuiper belt, Jupiter’s trojans, as well oblateness of the Sun and the relativistic Lense-Thirring effect. In addition, the influence of all these perturbations on the motion of the solar system planets is estimated and the regions in the solar system where the influence of these perturbations is most pronounced are given.},
  author = {E.~V. Pitjeva and D.~A. Pavlov and N.~P. Pitjev},
  doi = {10.32876/ApplAstron.51.82-92},
  issue = {51},
  journal = {Transactions of IAA RAS},
  keyword = {celestial mechanics, planet ephemerides, radar observations, asteroids, TNO, effects of General Relativity},
  pages = {82—92},
  title = {The Dynamic Model of the Solar System in the Planet Ephemerides EPM},
  url = {http://iaaras.ru/en/library/paper/2014/},
  year = {2019}
}

TY  - JOUR
TI  - The Dynamic Model of the Solar System in the Planet Ephemerides EPM
AU  - Pitjeva, E. V.
AU  - Pavlov, D. A.
AU  - Pitjev, N. P.
PY  - 2019
T2  - Transactions of IAA RAS
IS  - 51
SP  - 82
AB  - Currently, the accuracy of determining coordinates in the EPM
ephemeris is several meters for the inner planets and 10-20 meters
for Jupiter and Saturn. The need to build more accurate ephemeris of
planets requires improving the dynamic model of the solar system.
When constructing the ephemeris of the bodies of the solar system,
perturbations from the Sun, planets, and the Moon, as well as the
main relativistic effects are usually taken into account. The
perturbations of the next order of smallness , which also affect the
motion of the planets, are also considered in the paper. Such
perturbations are the the following: the attraction from the Main
asteroid belt, Kuiper belt, Jupiter’s trojans, as well oblateness of
the Sun and the relativistic Lense-Thirring effect. In addition, the
influence of all these perturbations on the motion of the solar
system planets is estimated and the regions in the solar system where
the influence of these perturbations is most pronounced are given.
DO  - 10.32876/ApplAstron.51.82-92
UR  - http://iaaras.ru/en/library/paper/2014/
ER  -