Ceres: Its Origin, Evolution and Structure and Dawn’s Potential Contribution

McCord, T. B.; Castillo‐Rogez, Julie; Rivkin, A. S.

doi:10.1007/s11214-010-9729-9

Cited by 49 publications

(11 citation statements)

References 39 publications

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“…Combining spherical harmonic coefficients from the anticipated shape models for Vesta and Ceres (Raymond et al 2011b) will allow long-wavelength estimates of interior structure (cf. McCord et al 2011;) posed in terms of crustal and elastic thicknesses or mantle density variations (Neumann et al 1996;Wieczorek 2007).…”

Section: Gravity Determination Techniquementioning

confidence: 99%

The Dawn Gravity Investigation at Vesta and Ceres

et al. 2011

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The objective of the Dawn gravity investigation is to use high precision X-band Doppler tracking and landmark tracking from optical images to measure the gravity fields of Vesta and Ceres to a half-wavelength surface resolution better than 90-km and 300-km, respectively. Depending on the Doppler tracking assumptions, the gravity field will be determined to somewhere between harmonic degrees 15 and 25 for Vesta and about degree 10 for Ceres. The gravity fields together with shape models determined from Dawn's framing camera constrain models of the interior from the core to the crust. The gravity field is determined jointly with the spin pole location. The second degree harmonics together with assumptions on obliquity or hydrostatic equilibrium may determine the moments of inertia.

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Section: Gravity Determination Techniquementioning

confidence: 99%

The Dawn Gravity Investigation at Vesta and Ceres

et al. 2011

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“…If this occurred, then small bodies that formed in the outer solar system may be found in the inner solar system (e.g., Levison et al 2009). For example, dwarf planet Ceres may have originated in the outer solar system and moved in during a dynamical instability (e.g., McKinnon 2008;McCord et al 2011;DeSanctis et al 2015). Should the largescale reorganization hypothesis prove true, it is likely that some small bodies in the inner solar system will have residual sulfuror nitrogen-containing compounds at their surfaces, as a tracer of this history.…”

Section: Introductionmentioning

confidence: 99%

Visible Near-infrared Spectral Evolution of Irradiated Mixed Ices and Application to Kuiper Belt Objects and Jupiter Trojans

Poston

Mahjoub

Ehlmann

et al. 2018

ApJ

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Understanding the history of Kuiper Belt Objects and Jupiter Trojans will help to constrain models of solar system formation and dynamical evolution. Laboratory simulations of a possible thermal and irradiation history of these bodies were conducted on ice mixtures while monitoring their spectral properties. These simulations tested the hypothesis that the presence or absence of sulfur explains the two distinct visible near-infrared spectral groups observed in each population and that Trojans and KBOs share a common formation location. Mixed ices consisting of water, methanol, and ammonia, in mixtures both with and without hydrogen sulfide, were deposited and irradiated with 10 keV electrons. Deposition and initial irradiation were performed at 50 K to simulate formation at 20 au in the early solar system, then heated to Trojan-like temperatures and irradiated further. Finally, irradiation was concluded and resulting samples were observed during heating to room temperature. Results indicated that the presence of sulfur resulted in steeper spectral slopes. Heating through the 140-200 K range decreased the slopes and total reflectance for both mixtures. In addition, absorption features at 410, 620, and 900 nm appeared under irradiation, but only in the H 2 S-containing mixture. These features were lost with heating once irradiation was concluded. While the results reported here are consistent with the hypothesis, additional work is needed to address uncertainties and to simulate conditions not included in the present work.

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“…The spacecraft DAWN should normally be placed in orbit around it in 2015. As for (4) Vesta, we expect precious data about its internal structure (McCord et al 2011). However, from ground-based observations and the Hubble Space Telescope, its shape is well defined, and we can already assume some solid hypotheses: with a mean radius of 467.6 ± 2.2 km, (1) Ceres has a spheroid shape with a small oblateness as terrestrial planets (Carry et al 2008).…”

Section: Parameters For (1) Ceresmentioning

confidence: 99%

High precision model of precession and nutation of the asteroids (1) Ceres, (4) Vesta, (433) Eros, (2867) Steins, and (25143) Itokawa

Petit¹,

Souchay²,

Lhotka³

2014

A&A

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Context. Several asteroids have recently been visited by spacecrafts that give us precious information and new constraints on their physical and rotational properties. In parallel, there are already several well-established theories to model the rotational motion of a rigid body, but accurate models of the rotational motion of asteroids have been poorly investigated so far. Aims. We aim to model the rotational motion of the asteroids (1) Ceres, (4) Vesta, (433) Eros, (2867) Steins, and (25143) Itokawa with high precision. Their physical parameters have been or will be (in the case of Ceres) better constrained by data from space missions. We concentrate in particular on the motion of their spin axis in space, a component that is generally not studied. Methods. We used Kinoshita's theory, based on a Hamiltonian approach for the rotation of a rigid body. We deduced an analytical model for determining the precession rate and the nutation coefficients for the set of five asteroids selected above. Results. For each asteroid considered we make a summary of the rotational and physical characteristics necessary for our calculations, and we give both the precession rate and accurate tables of nutation. Results show a very high precession rate for (25143) Itokawa, of more than one degree per decade (ψ = −(461.52 ± 6.57) /yr), and rather high ones for (433) Eros and (2867) Steins. We present the complete tables of nutation for both (1) Ceres and (4) Vesta, and give the peak-to-peak amplitudes for the five asteroids. At last, we show the curves described by the spin axis in space. Results agree with previous ones for (4)Vesta and (433) Eros. Conclusions. In this paper we show that it is possible to accurately compute the combined precession-nutation motion of asteroids that are well constrained by observational data as we do for a set of five asteroids. This enables one to understand the rotational behavior of their spin axis in space and constitutes an interesting step toward knowing of their rotational evolution and its consequences on their history. This work should serve as a basis for more extended ones dealing with the long-term rotational dynamics of the asteroids studied.

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Ceres: Its Origin, Evolution and Structure and Dawn’s Potential Contribution

Cited by 49 publications

References 39 publications

The Dawn Gravity Investigation at Vesta and Ceres

The Dawn Gravity Investigation at Vesta and Ceres

Visible Near-infrared Spectral Evolution of Irradiated Mixed Ices and Application to Kuiper Belt Objects and Jupiter Trojans

High precision model of precession and nutation of the asteroids (1) Ceres, (4) Vesta, (433) Eros, (2867) Steins, and (25143) Itokawa

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