Updated IAA RAS planetary ephemerides-EPM2011 and their use in scientific research

Solar System Research (Impact Factor: 0.65). 08/2013; 47(5). DOI: 10.1134/S0038094613040059
Source: arXiv


The EPM2011 ephemerides are computed using an updated dynamical model, new
values of the parameters, and an extended observation database that contains
about 680 000 positional measurements of various types obtained from 1913 to
2011. The dynamical model takes into account mutual perturbations of the major
planets, the Sun, the Moon, 301 massive asteroids, and 21 of the largest
trans-Neptunian objects (TNOs), as well as perturbations from the other
main-belt asteroids and other TNOs. The EPM ephemerides are computed by
numerical integration of the equations of motion of celestial bodies in the
parameterized post-Newtonian n-body metric in the BCRS coordinate system for
the TDB time scale over a 400-year interval. The ephemerides were oriented to
the ICRF system using 213 VLBI observations (taken from 1989 to 2010) of
spacecraft near planets with background quasars, the coordinates of which are
given in the ICRF system. The accuracy of the constructed ephemerides was
verified by comparison with observations and JPL independent ephemerides DE424.
The EPM ephemerides are used in astronavigation (they form the basis of the
{\it Astronomical Yearbook} and are planned to be utilized in GLONASS and
LUNA-RESURS programs) and various research, including the estimation of the
solar oblateness, the parameters of the rotation of Mars, and the total mass of
the asteroid main belt and TNOs, as well as the verification of general
relativity, the secular variations of the Sun's mass and the gravitational
constant, and the limits on the dark matter density in the Solar System.
The EPM ephemerides, together with the corresponding time differences TT -
TDB and the coordinates of seven additional objects (Ceres, Pallas, Vesta,
Eris, Haumea, Makemake, and Sedna), are available at

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    European Physical Journal C 03/2015; 75(5). DOI:10.1140/epjc/s10052-015-3394-9 · 5.08 Impact Factor
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    ABSTRACT: We here apply the ASTG-model to the observed anomalous secular trend in the mean Sun-(Earth-Moon) and Earth-Moon distances. For the recession of the Earth-Moon system, in agreement with observation, we obtain a recession of about 11.20 ± 0.20 cm/yr. The ASTG-model predicts orbital drift as being a result of the orbital inclination and the Solar mass loss rate. The Newtonian gravitational constant G is assumed to be absolute time constant. Standish (2005); Krasinsky and Brumberg (2004) reported for the Earth-Moon system, an orbital recession from the Sun of about (15.00 ± 4.00) cm/yr; while Williams et al. (2004); Williams and Boggs (2009); Williams et al. (2014) report for the Moon, an orbital recession of about 38.00 mm/yr from the Earth. The predictions of the ASTG-model for the Earth-Moon system agrees very well with those the findings of Standish (2005); Krasinsky and Brumberg (2004). The lost orbital angular momen-tum for the Earth-Moon system – which we here hypothesize to be gained as spin by the two body Earth-Moon system; this lost angular momentum accounts very well for the observed lunar drift, therefore, one can safely safely say that the ASTG-model does to a reasonable degree of accuracy predict the observed lunar drift of about 38.00 mm/yr from the Earth.
    Astrophysics and Space Science 11/2014; DOI:10.1007/s10509-015-2394-4 · 2.26 Impact Factor
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    • "In regard to the anomalous and extra-anomalous perihelion precession, what can the ASTG-model be applied to. This question we ask after having tried (and failed) to model using the ASTG-model, the extra-anomalous perihelion precessions that have been measured by Fienga et al. (2011b); Pitjeva and Pitjev (2013). This effort we conducted as part and parcel of the package of recommendations by the anonymous reviewer. "
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    Monthly Notices of the Royal Astronomical Society 09/2014; 1:1-6. DOI:10.1093/mnras/stv1100 · 5.11 Impact Factor
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