Detailed Solar System dynamics as a probe of the Dark Matter hypothesis

Hernández, X.

doi:10.48550/arxiv.1901.10605

Cited by 4 publications

(12 citation statements)

References 26 publications

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“…Our results in Figure 2 are much smaller than those obtained by Hernandez (2019). This is because we properly take the resonant limit of Equation 21while Hernandez (2019) found the maximum amplitude of the induced perturbations. This maximum is reached after order the Galactic orbital period of the Sun.…”

Section: Comparison With Hernandez (2019)contrasting

confidence: 62%

“…If the observed dynamical discrepancies are due to DM, then massive objects moving through the Galactic DM halo should experience dynamical friction (Chandrasekhar 1943). This is also true for the Sun, which would be expected to create a trailing DM wake (Hernandez 2019). Because the DM would be overdense behind the Sun, its distribution would not be spherically symmetric, contrary to the assumption of several previous works (e.g.…”

Section: Introductionmentioning

confidence: 84%

“…For a much shorter observing duration, the maximum possible amplitude of δr is not relevant. The fact that this is only a few hundred metres (Hernandez 2019) shows just how little the DM wake would really influence the Solar System.…”

Section: Comparison With Hernandez (2019)mentioning

confidence: 99%

“…Such an effect is not seen in Cassini radio tracking data despite it being accurate to 32 metres (Viswanathan et al 2017). This led Hernandez (2019) to rule out the DM hypothesis.…”

Section: Introductionmentioning

confidence: 99%

“…This asymmetry might allow for much stronger constraints on the DM density. Following this idea, Hernandez (2019) found that the Sun's DM wake would cause the position of Saturn to deviate by 252 metres. Such an effect is not seen in Cassini radio tracking data despite it being accurate to 32 metres (Viswanathan et al 2017).…”

Section: Introductionmentioning

confidence: 99%

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Effect of the Solar dark matter wake on planets

Banik

Kroupa

2019

Monthly Notices of the Royal Astronomical Society

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The Galaxy is conventionally thought to be surrounded by a massive dark matter (DM) halo. As the Sun goes through this halo, it excites a DM wake behind it. This local asymmetry in the DM distribution would gravitationally affect the motions of Solar System planets, potentially allowing the DM wake to be detected or ruled out. Hernandez (2019) recently calculated that the DM-induced perturbation to Saturn's position is 252 metres net of the effect on the Sun. No such anomaly is seen in Saturn's motion despite very accurate tracking of the Cassini spacecraft, which orbited Saturn for >13 years.Here, we revisit the calculation of how much Saturn would deviate from Keplerian motion if we fix its position and velocity at some particular time. The DM wake induces a nearly resonant perturbation whose amplitude grows almost linearly with time. We show that the Hernandez (2019) result applies only for an observing duration comparable to the ≈ 250 million year period of the Sun's orbit around the Galaxy. Over a 100 year period, the perturbation to Saturn's orbit amounts to <1 cm, which is quite consistent with existing observations. Even smaller perturbations are expected for the terrestrial planets.

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Section: Comparison With Hernandez (2019)contrasting

confidence: 62%

Section: Introductionmentioning

confidence: 84%

Section: Comparison With Hernandez (2019)mentioning

confidence: 99%

“…Such an effect is not seen in Cassini radio tracking data despite it being accurate to 32 metres (Viswanathan et al 2017). This led Hernandez (2019) to rule out the DM hypothesis.…”

Section: Introductionmentioning

confidence: 99%

Section: Introductionmentioning

confidence: 99%

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Effect of the Solar dark matter wake on planets

Banik

Kroupa

2019

Monthly Notices of the Royal Astronomical Society

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Are the planetary orbital effects of the solar dark matter wake detectable?

Iorio

2019

Monthly Notices of the Royal Astronomical Society

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Recently, there has been some discussion in the literature about the effects of the anisotropy in the spatial density of dark matter in the Solar neighbourhood arising from the motion of the Sun through the Galactic halo. In particular, questions have been asked about the orbital motions of the solar system's planets and whether these motions can be effectively constrained by the radiotechnical observations collected by Cassini. I show that the semilatus rectum p, the eccentricity e, the inclination I, the longitude of the ascending node Ω, the longitude of perihelion ̟, and the mean anomaly at epoch η of a test particle of a restricted two-body system affected by the gravity of a dark matter wake undergo secular rates of change. In the case of Saturn, they are completely negligible, being at the order of ≃ 0.1 millimeter per century and ≃ 0.05−2 nanoarcseconds per century: the current (formal) accuracy level in constraining any anomalous orbital precessions is of the order of ≃ 0.002−2 milliarcseconds per century for Saturn. I also numerically simulate the Earth-Saturn range signature ∆ρ(t) due to the dark matter wake over the same time span (2004)(2005)(2006)(2007)(2008)(2009)(2010)(2011)(2012)(2013)(2014)(2015)(2016)(2017) as covered by the Cassini data record. I find that it is as low as ≃ 0.1 − 0.2 m, while the existing range residuals, computed by astronomers without modeling any dark matter wake effect, are of the order of ≃ 30 m. The local dark matter density ̺ DM would need to be larger than the currently accepted value of ̺ DM = 0.018 M ⊙ pc −3 by a factor of 2.5 × 10 6 in order to induce a geocentric Kronian range signature large enough to make it discernible in the present-day residuals.keywords ephemerides -celestial mechanics -space vehicles -dark matter -gravitationplanets and satellites: dynamical evolution and stability

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The Case for a Large-scale Occultation Network

Rice¹,

Laughlin²

2019

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We discuss the feasibility of and present initial designs and approximate cost estimates for a large (N ∼ 2000) network of small photometric telescopes that is purpose-built to monitor V 15 Gaia Mission program stars for occultations by minor solar system bodies. The implementation of this network would permit measurement of the solar system's tidal gravity field to high precision, thereby revealing the existence of distant trans-Neptunian objects such as the proposed "Planet Nine." As a detailed example of the network capabilities, we investigate how occultations by Jovian Trojans can be monitored to track the accumulation of gravitational perturbations, thereby constraining the presence of undetected massive solar system bodies. We also show that the tidal influence of Planet Nine can be discerned from that of smaller, nearer objects in the Kuiper belt. Moreover, ephemerides for all small solar system bodies observed in occultation could be significantly improved using this network, thereby improving spacecraft navigation and refining Solar System modeling. Finally, occultation monitoring would generate direct measurements of size distributions for asteroid populations, permitting a better understanding of their origins.

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Detailed Solar System dynamics as a probe of the Dark Matter hypothesis

Cited by 4 publications

References 26 publications

Effect of the Solar dark matter wake on planets

Effect of the Solar dark matter wake on planets

Are the planetary orbital effects of the solar dark matter wake detectable?

The Case for a Large-scale Occultation Network

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