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Construction of the numerical motion theories for the main satellites of Mars, Jupiter, Saturn and Uranus in IAA RAS

A. Poroshina, M. Zamarashkina, G. Kosmdamianskiy

Transactions of IAA RAS, issue 26, 75–87 (2012)

Keywords: satellite, major planet, oblateness, numerical integration

Abstract

This paper presents the motion theories of the main satellites of Mars (Phobos, Deimos), Jupiter (Io, Europa, Ganymede, Callisto), Saturn (Mimas, Enceladus, Tethys, Dione, Rhea, Titan, Hyperion, Iapetus), and Uranus (Ariel, Umbriel, Titania, Oberon, Miranda) as constructed by numerical integration within the framework of the program package ERA (Ephemeris Research in Astronomy). The dynamical models include the mutual perturbations of the satellites, disturbances of the Sun, major planets and oblateness of the central planet (). For the Phobos motion, the tidal perturbations from Mars are taken into account. The initial values of the coordinates and velocities were using the astrometric observations of different types. In addition, several improved parameters (the planet mass, and pole coordinates, the masses of the satellites) were improved for some satellite systems. The residuals, rms and comparison of our results with those obtained by other authors are given.

Citation

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A. Poroshina, M. Zamarashkina, G. Kosmdamianskiy. Construction of the numerical motion theories for the main satellites of Mars, Jupiter, Saturn and Uranus in IAA RAS // Transactions of IAA RAS. — 2012. — Issue 26. — P. 75–87.

@article{poroshina2012,
  abstract = {This paper presents the motion theories of the main satellites of Mars (Phobos, Deimos), Jupiter (Io, Europa, Ganymede, Callisto), Saturn (Mimas, Enceladus, Tethys, Dione, Rhea, Titan, Hyperion, Iapetus), and Uranus (Ariel, Umbriel, Titania, Oberon, Miranda) as constructed by numerical integration within the framework of the program package ERA (Ephemeris Research in Astronomy). The dynamical models include the mutual perturbations of the satellites, disturbances of the Sun, major planets and oblateness of the central planet (). For the Phobos motion, the tidal perturbations from Mars are taken into account. The initial values of the coordinates and velocities were using the astrometric observations of different types. In addition, several improved parameters (the planet mass, and pole coordinates, the masses of the satellites) were improved for some satellite systems. The residuals, rms and comparison of our results with those obtained by other authors are given.},
  author = {A. Poroshina and M. Zamarashkina and G. Kosmdamianskiy},
  issue = {26},
  journal = {Transactions of IAA RAS},
  keyword = {satellite, major planet, oblateness, numerical integration},
  pages = {75--87},
  title = {Construction of the numerical motion theories for the main satellites of Mars, Jupiter, Saturn and Uranus in IAA RAS},
  url = {http://iaaras.ru/en/library/paper/900/},
  year = {2012}
}

TY  - JOUR
TI  - Construction of the numerical motion theories for the main satellites of Mars, Jupiter, Saturn and Uranus in IAA RAS
AU  - Poroshina, A.
AU  - Zamarashkina, M.
AU  - Kosmdamianskiy, G.
PY  - 2012
T2  - Transactions of IAA RAS
IS  - 26
SP  - 75
AB  -  This paper presents the motion theories of the main satellites of
Mars (Phobos, Deimos), Jupiter (Io, Europa, Ganymede, Callisto),
Saturn (Mimas, Enceladus, Tethys, Dione, Rhea, Titan, Hyperion,
Iapetus), and Uranus (Ariel, Umbriel, Titania, Oberon, Miranda) as
constructed by numerical integration within the framework of the
program package ERA (Ephemeris Research in Astronomy). The dynamical
models include the mutual perturbations of the satellites,
disturbances of the Sun, major planets and oblateness of the central
planet (). For the Phobos motion, the tidal perturbations from Mars
are taken into account. The initial values of the coordinates and
velocities were using the astrometric observations of different
types. In addition, several improved parameters (the planet mass, and
pole coordinates, the masses of the satellites) were improved for
some satellite systems. The residuals, rms and comparison of our
results with those obtained by other authors are given.
UR  - http://iaaras.ru/en/library/paper/900/
ER  -