The Perihelion Precession of Saturn, Planet X/Nemesis and MOND~!2009-09-17~!2009-10-08~!2010-05-05~!

Iorio, Lorenzo

doi:10.2174/1874381101003010001

Cited by 25 publications

(13 citation statements)

References 20 publications

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“…[32] has put forth a different form for the planetary EFE yielding an additional quadrupolar extra-acceleration which mimics the action of distant mass; some consequences have been investigated in Ref. [33].…”

Section: The External Field Effect In Mondmentioning

confidence: 99%

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MOND Orbits in the Oort Cloud

Iorio¹

2010

TOAAJ

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We numerically investigate the features of typical orbits occurring in the Oort cloud (r ≈ 50 − 150 kAU) in the low-acceleration regime of the MOdified Newtonian Dynamics (MOND). We fully take into account the so-called External Field Effect (EFE) because the solar system is embedded in the Milky Way. In the framework of MOND this does matter since the gravitational acceleration of Galactic origin felt by the solar system is of the same order of magnitude of the characteristic MOND acceleration scale A 0 ≈ 10 −10 m s −2 . We use three different forms of the MOND interpolating function µ(x), two different values for the Galactic field at the Sun's location and different initial conditions corresponding to plausible Keplerian ellipses in the Oort cloud. We find that MOND produces highly distorted trajectories with respect to the Newtonian case, especially for very eccentric orbits. It turns out that the shape of the MOND orbits strongly depend on the initial conditions. For particular initial state vectors, the MOND paths in the ecliptic plane get shrunk extending over much smaller spatial regions than in the Newtonian case, and experience high frequency variations over one Keplerian orbital period. Ecliptic orbits with different initial conditions and nearly polar orbits are quite different getting distorted as well, but they occupy more extended spatial regions. These facts may have consequences on the composition and the dynamical history of the Oort cloud which are difficult to predict in detail; certainly, the MOND picture of the Oort region is quite different from the Newtonian one exhibiting no regularities.

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Section: The External Field Effect In Mondmentioning

confidence: 99%

“…For other works on MOND in the inner regions of the solar system, see Ref. [4,22,23,24,25,26,27,28,32,33].…”

Section: Introductionmentioning

confidence: 99%

MOND Orbits in the Oort Cloud

Iorio¹

2010

TOAAJ

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“…= GM X /r 3 X according to the anomalous perihelion precession of Saturn analyzed in Ref. 40 a genuine physical effect h . The maximum effect of X on the Mercury range would be as large as 1.5 − 3 m, falling within the measurability domain of BepiColombo.…”

Section: Planet Xmentioning

confidence: 97%

Effects of Standard and Modified Gravity on Interplanetary Ranges

Iorio

2011

Int. J. Mod. Phys. D

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We numerically investigate the impact on the two-body range of several Newtonian and non-Newtonian dynamical effects for some Earth-planet (Mercury, Venus, Mars, Jupiter, Saturn) pairs, in view of the expected cm-level accuracy in some future planned or proposed interplanetary ranging operations. The general relativistic gravitomagnetic Lense-Thirring effect should be modeled and solved for in future accurate ranging tests of Newtonian and post-Newtonian gravity, because it falls within their measurability domain. It could a priori "imprint" the determination of some of the target parameters of the tests considered. Moreover, the ring of the minor asteroids, Ceres, Pallas, Vesta (and also many other asteroids if Mars is considered) and the trans-Neptunian objects (TNOs) act as sources of nonnegligible systematic uncertainty on the larger gravitoelectric post-Newtonian signals from which it is intended to determine the parameters γ and β of the parametrized post-Newtonian (PPN) formalism with very high precision (several orders of magnitude better than the current 10 −4 -10 −5 levels). Also, other putative, nonconventional gravitational effects, like a violation of the strong equivalence principle (SEP), a secular variation of the Newtonian constant of gravitation G, and the Pioneer anomaly, are considered. The presence of a hypothetical, distant planetary-sized body X could be detectable with future high-accuracy planetary ranging. Our analysis can, in principle, be extended to future interplanetary ranging scenarios in which one or more spacecrafts in heliocentric orbits are involved. The impact of fitting the initial conditions, and of the noise in the observations, on the actual detectability of the dynamical signatures investigated, which may be partly absorbed in the estimation process, should be quantitatively addressed in further studies. a See http://meetingorganizer.copernicus.org/EPSC2010/EPSC2010-60.pdf b It is an ESA mission, including two spacecraft, one of them provided by Japan, to be put into orbit around Mercury. The launch is scheduled for 2014. The construction of the instruments is currently ongoing. Int. J. Mod. Phys. D 2011.20:181-232. Downloaded from www.worldscientific.com by TUBITAK NATIONAL OBSERVATORY (TUG) on 02/04/15. For personal use only. c Its cheaper version, ASTROD I, makes use of one spacecraft in a Venus-gravity-assisted solar orbit, ranging optically with ground stations. 16 Int. J. Mod. Phys. D 2011.20:181-232. Downloaded from www.worldscientific.com by TUBITAK NATIONAL OBSERVATORY (TUG) on 02/04/15. For personal use only. 184 L. Iorioand mean equinox of the reference epoch, i.e. J2000.0, centered at the solar system barycenter (SSB); the initial conditions at the epoch J2000.0 were retrieved with the HORIZONS WEB interface by JPL, NASA. The temporal interval of the numerical integration for Mercury and Venus has been taken equal to ∆t = 2 yr, in view of the fact that the typical operational time spans envisaged for the future PLR technique are similar. For Mars and Saturn, f...

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“…• Iorio (2010) found that a distant, pointlike massive object in the outer regions of the solar system may explain the anomalous retrograde precession 1 of the perihelion of Saturn preliminarily estimated (Pitjeva 2008) by analyzing some radiotechnical data points from the Cassini spacecraft exploring the Saturnian system.…”

Section: Introductionmentioning

confidence: 98%

“…Have not the remote peripheries of the solar system saved any further big surprises for us? It is a long time (Lowell 1915;Pickering 1928Pickering , 1931Schuette 1949) that such questions−still well alive (Lykawka and Mukai 2008;Iorio 2010;Matese and Whitmire 2011;Fernández 2011)−are well rooted in the astronomical community, having often resurfaced in different contexts and with changed forms;. For a recent, popular review, see Schilling (2009).…”

Section: Introductionmentioning

confidence: 99%

Constraints on the location of a putative distant massive body in the Solar System from recent planetary data

Iorio

2011

Celest Mech Dyn Astr

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We analytically work out the long-term variations caused on the motion of a planet orbiting a star by a very distant, pointlike massive object X. Apart from the semi-major axis a, all the other Keplerian osculating orbital elements experience long-term variations which are complicated functions of the orbital configurations of both the planet itself and of X. We infer constraints on the minimum distance d X at which X may exist by comparing our prediction of the long-term variation of the longitude of the perihelion to the latest empirical determinations of the corrections ˙ to the standard Newtonian/Einsteinian secular precessions of several solar system planets recently estimated by independent teams of astronomers. We obtain the following approximate lower bounds on d X for the assumed masses of X quoted in brackets: 150-200 au (Mars), 250-450 au (0.7 m ⊕ ), 3500-4500 au (4 m Jup ).

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The Perihelion Precession of Saturn, Planet X/Nemesis and MOND~!2009-09-17~!2009-10-08~!2010-05-05~!

Cited by 25 publications

References 20 publications

MOND Orbits in the Oort Cloud

MOND Orbits in the Oort Cloud

Effects of Standard and Modified Gravity on Interplanetary Ranges

Constraints on the location of a putative distant massive body in the Solar System from recent planetary data

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