Galilean satellite ephemerides E5

Lieske, J. H.

doi:10.1051/aas:1998182

Cited by 73 publications

(61 citation statements)

References 24 publications

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“…3 for the mutual event observations, with those presented in Lieske (1998) and Kaas et al (1999). One notes that the (O-C)s resulting from our model are much lower, especially for the campaign of 1991.…”

Section: The (O-c)smentioning

confidence: 55%

New accurate ephemerides for the Galilean satellites of Jupiter

Lainey

Arlot

Vienne

2004

A&A

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Abstract. We present a new model of the four Galilean satellites Io, Europa, Ganymede and Callisto, able to deliver accurate ephemerides over a very long time span (several centuries). In the first paper (Lainey et al. 2004(Lainey et al. , A&A, 420, 1171 we gave the equations of the dynamical model. Here we present the fit of this model to the observations, covering more than one century starting from 1891. Our ephemerides, based on this first fit called L1, are available on the web page of the IMCCE at the URL

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Section: The (O-c)smentioning

confidence: 55%

New accurate ephemerides for the Galilean satellites of Jupiter

Lainey

Arlot

Vienne

2004

A&A

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“…The orbital studies of these celestial bodies demand the observation of positions, relative distances or other forms of observables, like central instants and impact parameters in mutual phenomena, over extended period of time to fit them with dynamic models (De Sitter 1928;Lieske 1987;Lainey et al 2009). However, to detect very weak disturbance forces, such as tidal forces, these observables have to be very precise.…”

Section: Introductionmentioning

confidence: 99%

Astrometry of mutual approximations between natural satellites. Application to the Galilean moons

Morgado

Assafin

Vieira-Martins

et al. 2016

Mon. Not. R. Astron. Soc.

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Typically we can deliver astrometric positions of natural satellites with errors in the 50-150 mas range. Apparent distances from mutual phenomena, have much smaller errors, less than 10 mas. However, this method can only be applied during the equinox of the planets. We developed a method that can provide accurate astrometric data for natural satellites -the mutual approximations. The method can be applied when any two satellites pass close by each other in the apparent sky plane. The fundamental parameter is the central instant t 0 of the passage when the distances reach a minimum.We applied the method for the Galilean moons. All observations were made with a 0.6 m telescope with a narrow-band filter centred at 889 nm with width of 15 nm which attenuated Jupiter's scattered light. We obtained central instants for 14 mutual approximations observed in 2014-2015. We determined t 0 with an average precision of 3.42 mas (10.43 km). For comparison, we also applied the method for 5 occultations in the 2009 mutual phenomena campaign and for 22 occultations in the 2014-2015 campaign. The comparisons of t 0 determined by our method with the results from mutual phenomena show an agreement by less than 1-sigma error in t 0 , typically less than 10 mas. This new method is particularly suitable for observations by small telescopes.

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“…From our observed events, we have been able to calculate the drift in the longitude of satellites J1 and J2 from the three events involving J1 and J2 based on different theoretical models: L2 (2009) and L1 (2006) by Lainey, G5 by Arlot (1982) and E5 by Lieske (1998). During one event, the difference between the observed longitude and the calculated one depended on the difference between the observed mid-time and the calculated one through Eq.…”

Section: Discussion and Interpretationmentioning

confidence: 99%

Mutual occultations between Galilean satellites observed at Yunnan Observatory in 2009

Zhang

Arlot

Liu

2011

A&A

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Context. Photometry of mutual events between natural satellites has been shown to be a most effective and accurate ground-based method for obtaining accurate astrometric data by fitting the light curves observed during these events, and is invaluable for developing the orbital models of the natural satellites. (Nov. 28, 2009) were observed at Yunnan Observatory during the PHEMU09 international campaign. We calculate the astrometric data of satellites by analyzing and fitting the light curves that we derived. Methods. The model proposed by Emelianov (2003, Sol. Syst. Res., 37, 314) was used to fit the light curves, while taking the LommelSeeliger scattering law into account. Results. For each event, we derive dynamical quantities such as the deviation of the observed relative satellite motion from the theoretical motion provided by the relevant ephemeris denoted as D x and D y , and the impact parameter and its corresponding midtime. These results have an accuracy of between about several mas and 90 mas for D x and D y , and 0.31-2.97 s for the mid-time. The residuals of the longitude shifts (δl 1 for J1 Io and δl 2 for J2 Europa) that represent the shifts of the mid-times of the events, are also calculated to be around 10 km with the most accurate available ephemerides.

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Galilean satellite ephemerides E5

Cited by 73 publications

References 24 publications

New accurate ephemerides for the Galilean satellites of Jupiter

New accurate ephemerides for the Galilean satellites of Jupiter

Astrometry of mutual approximations between natural satellites. Application to the Galilean moons

Mutual occultations between Galilean satellites observed at Yunnan Observatory in 2009

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