Project SEE (Satellite Energy Exchange): proposal for space-based gravitational measurements

Sanders, Alvin J.; Alexeev, A. D.; Allison, S. W.; Бронников, К. А.; Campbell, J. W.; Cates, M.R.; Corcovilos, Theodore A.; Earl, Duncan; Gadfort, T; Gillies, G. T.; Harris, Matthew L.; Kolosnitsyn, N. I.; Konstantinov, M. Yu.; Melnikov, V. N.; Newby, J.; Schunk, Richard G.; Smalley, Larry L.

doi:10.1088/0957-0233/10/6/317

Cited by 22 publications

(14 citation statements)

References 23 publications

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“…In principle, a rather unconventional possibility could be the realization of an artificial mini-planetary system to be carried onboard a drag-free spacecraft orbiting, say, the Earth; such an idea was already proposed in the past to accurately measure the Newtonian constant of gravitation G [48,49,50,51,52,53,54], and, more recently, to put on the test the MOND theory [55]. The conditions of validity of the present analysis could be fulfilled, e.g., by placing a non-rotating sphere made of tungsten with density ρ W = 19.6 g cm −3 and M = 28 kg, R = 7 cm inside a drag-free spacecraft orbiting the Earth in some suitably chosen High Earth Orbit (HEO).…”

Section: Post-newtonian Orbital Tidal Effects 4 Possible Scenarios Ofmentioning

confidence: 99%

Orbital motions as gradiometers for post-Newtonian tidal effects

Iorio¹

2014

Front. Astron. Space Sci.

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The direct long-term changes occurring in the orbital dynamics of a local gravitationally bound binary system S due to the post-Newtonian tidal acceleration caused by an external massive source are investigated. A class of systems made of a test particle m rapidly orbiting with orbital frequency n b an astronomical body of mass M which, in turn, slowly revolves around a distant object of mass M with orbital frequency n b n b is considered. The characteristic frequencies of the non-Keplerian orbital variations of m and of M itself are assumed to be negligible with respect to both n b and n b . General expressions for the resulting Newtonian and post-Newtonian tidal orbital shifts of m are obtained. The future missions BepiColombo and JUICE to Mercury and Ganymede, respectively, are considered in view of a possible detection. The largest effects, of the order of ≈ 0.1 − 0.5 milliarcseconds per year (mas yr −1 ), occur for the Ganymede orbiter of the JUICE mission. Although future improvements in spacecraft tracking and orbit determination might, perhaps, reach the required sensitivity, the systematic bias represented by the other known orbital perturbations of both Newtonian and post-Newtonian origin would be overwhelming. The realization of a dedicated artificial mini-planetary system to be carried onboard and Earth-orbiting spacecraft is considered as well. Post-Newtonian tidal precessions as large as ≈ 1 − 10 2 mas yr −1 could be obtained, but the quite larger Newtonian tidal effects would be a major source of systematic bias because of the present-day percent uncertainty in the product of the Earth's mass times the Newtonian gravitational parameter.

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Section: Post-newtonian Orbital Tidal Effects 4 Possible Scenarios Ofmentioning

confidence: 99%

Orbital motions as gradiometers for post-Newtonian tidal effects

Iorio¹

2014

Front. Astron. Space Sci.

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“…Modern theories are expected to make predictions in the range of ≈ 10 −13 yr −1 < Δ|Ġ/G| 10 −11 yr −1 (2) or somewhat less. The planned Satellite Energy Exchange (SEE) mission proposed originally by Sanders and Deeds [29][30][31] and discussed further by several others [32][33][34][35][36][37][38][39][40][41][42][43][44] has a design goal of measuring Δ|Ġ/G| to within ≈ 10 −14 yr −1 .…”

Section: Present Experimental Status Ofġmentioning

confidence: 99%

Implications upon theory discrimination of an accurate measurement of the time rate of change of the gravitational “constant” G and other cosmological parameters

2010

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A substantial improvement in the accuracy ofĠ tests (The dot denotes the time derivative.) would make it realistic to speak in terms of a measurement ofĠ, rather than merely a smaller upper bound on |Ġ|. We show that the accuracy Δ|Ġ/G| ≈ 10 −14 yr −1 may be sufficient, given the accuracy of other cosmological parameters, to observe effects predicted by higher dimensions theories and, hence, to discriminate among different models. TheĠ design goal for the SEE (Satellite Energy Exchange) mission is Δ(Ġ/G) ≈ 10 −14 yr −1 .

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“…The field, however, is heavier than in standard quintessence models (m cham ≫ H). In the solar system, where the density is many orders of magnitude smaller than on Earth, the chameleon is essentially a free field and mediates a long range force which could be detected by upcoming satellite experiments [6].…”

Section: Introductionmentioning

confidence: 99%

Small scale structure formation in chameleon cosmology

et al. 2006

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Chameleon fields are scalar fields whose mass depends on the ambient matter density. We investigate the effects of these fields on the growth of density perturbations on sub-galactic scales and the formation of the first dark matter halos. Density perturbations on comoving scales R < 1pc go non-linear and collapse to form structure much earlier than in standard ΛCDM cosmology. The resulting mini-halos are hence more dense and resilient to disruption. We therefore expect (provided that the density perturbations on these scales have not been erased by damping processes) that the dark matter distribution on small scales would be more clumpy in chameleon cosmology than in the ΛCDM model.

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Project SEE (Satellite Energy Exchange): proposal for space-based gravitational measurements

Cited by 22 publications

References 23 publications

Orbital motions as gradiometers for post-Newtonian tidal effects

Orbital motions as gradiometers for post-Newtonian tidal effects

Implications upon theory discrimination of an accurate measurement of the time rate of change of the gravitational “constant” G and other cosmological parameters

Small scale structure formation in chameleon cosmology

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