The thermal conductivity of meteorites: New measurements and analysis

Opeil, Cyril; Consolmagno, G. J.; Britt, D. T.

doi:10.1016/j.icarus.2010.01.021

Cited by 152 publications

(244 citation statements)

References 17 publications

(28 reference statements)

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“…Assuming values of heat capacity and material density typical of H5 ordinary chondrites (Opeil et al, 2010) and estimated surface temperature of 230 K and 180 K at 1.94 and 2.87 AU respectively, we find that the typical grain size of Hebe is about 0.2-0.3 mm (see Annexe B for more details).…”

Section: Thermal Parameters and Regolith Grain Sizementioning

confidence: 93%

3D shape of asteroid (6) Hebe from VLT/SPHERE imaging: Implications for the origin of ordinary H chondrites

Marsset

Carry

Dumas

et al. 2017

A&A

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Context. The high-angular-resolution capability of the new-generation ground-based adaptive-optics camera SPHERE at ESO VLT allows us to assess, for the very first time, the cratering record of medium-sized (D∼100-200 km) asteroids from the ground, opening the prospect of a new era of investigation of the asteroid belt's collisional history. Aims. We investigate here the collisional history of asteroid (6) Hebe and challenge the idea that Hebe may be the parent body of ordinary H chondrites, the most common type of meteorites found on Earth (∼34% of the falls). Methods. We observed Hebe with SPHERE as part of the science verification of the instrument. Combined with earlier adaptiveoptics images and optical light curves, we model the spin and three-dimensional (3D) shape of Hebe and check the consistency of the derived model against available stellar occultations and thermal measurements. Results. Our 3D shape model fits the images with sub-pixel residuals and the light curves to 0.02 mag. The rotation period (7.274 47 h), spin (ECJ2000 λ,β of 343 • ,+47 • ), and volume-equivalent diameter (193 ± 6 km) are consistent with previous determinations and thermophysical modeling. Hebe's inferred density is 3.48 ± 0.64 g.cm −3 , in agreement with an intact interior based on its H-chondrite composition. Using the 3D shape model to derive the volume of the largest depression (likely impact crater), it appears that the latter is significantly smaller than the total volume of close-by S-type H-chondrite-like asteroid families. Conclusions. Our results imply that (6) Hebe is not the most likely source of H chondrites. Over the coming years, our team will collect similar high-precision shape measurements with VLT/SPHERE for ∼40 asteroids covering the main compositional classes, thus providing an unprecedented dataset to investigate the origin and collisional evolution of the asteroid belt.

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Section: Thermal Parameters and Regolith Grain Sizementioning

confidence: 93%

3D shape of asteroid (6) Hebe from VLT/SPHERE imaging: Implications for the origin of ordinary H chondrites

Marsset

Carry

Dumas

et al. 2017

A&A

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“…In addition, we used the physical properties (thermal conductivity, specific heat and density) for ice, water 60,61 and rock 62,63 , detailed in Supplementary Table 6 (part 3).…”

Section: Methodsmentioning

confidence: 99%

Early aqueous activity on the ordinary and carbonaceous chondrite parent bodies recorded by fayalite

et al. 2015

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Chronology of aqueous activity on chondrite parent bodies constrains their accretion times and thermal histories. Radiometric 53 Cr dating has been successfully applied to aqueously formed carbonates in CM carbonaceous chondrites. Owing to the absence of carbonates in ordinary (H, L and LL), and CV and CO carbonaceous chondrites, and the lack of proper standards, there are no reliable ages of aqueous activity on their parent bodies. Here we report the first 53 Mn-53 Cr ages of aqueously formed fayalite in the L3 chondrite Elephant Moraine 90161 as 2:4 þ 1:8 À 1:3 Myr after calcium-aluminium-rich inclusions (CAIs), the oldest Solar System solids. In addition, measurements using our synthesized fayalite standard show that fayalite in the CV3 chondrite Asuka 881317 and CO3-like chondrite MacAlpine Hills 88107 formed 4:2 þ 0:8 À 0:7 and 5:1 þ 0:5 À 0:4 Myr after CAIs, respectively. Thermal modelling, combined with the inferred conditions (temperature and water/rock ratio) and 53 Cr ages of aqueous alteration, suggests accretion of the L, CV and CO parent bodies B1.8 À 2.5 Myr after CAIs.

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“…Such high values are suspicious because they are significantly higher than measured for any other asteroid . In addition, Opeil et al (2010) provided upper limits for Γ of CM and CK4 chondritic meteorite materials, both proposed as likely analogs of Phaethon. Thermal inertia values for either CM (<650 J m −2 s −1/2 K −1 ) and CK4 (<1400 J m −2 s −1/2 K −1 ) are much lower than our lower limit of ∼2000 J m −2 s −1/2 K −1 derived for the second pole solution.…”

Section: Thermophysical Properties and Sizementioning

confidence: 99%

Near-Earth asteroid (3200) Phaethon: Characterization of its orbit, spin state, and thermophysical parameters

Hanuš

Delbò

Vokrouhlický

et al. 2016

A&A

110

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Context. The near-Earth asteroid (3200) Phaethon is an intriguing object: its perihelion is at only 0.14 au and is associated with the Geminid meteor stream. Aims. We aim to use all available disk-integrated optical data to derive a reliable convex shape model of Phaethon. By interpreting the available space-and ground-based thermal infrared data and Spitzer spectra using a thermophysical model, we also aim to further constrain its size, thermal inertia, and visible geometric albedo. Methods. We applied the convex inversion method to the new optical data obtained by six instruments and to previous observations. The convex shape model was then used as input for the thermophysical modeling. We also studied the long-term stability of Phaethon's orbit and spin axis with a numerical orbital and rotation-state integrator.Results. We present a new convex shape model and rotational state of Phaethon: a sidereal rotation period of 3.603958(2) h and ecliptic coordinates of the preferred pole orientation of (319 • , −39 • ) with a 5 • uncertainty. Moreover, we derive its size (D = 5.1 ± 0.2 km), thermal inertia (Γ = 600 ± 200 J m −2 s −1/2 K −1 ), geometric visible albedo (p V = 0.122 ± 0.008), and estimate the macroscopic surface roughness. We also find that the Sun illumination at the perihelion passage during the past several thousand years is not connected to a specific area on the surface, which implies non-preferential heating.

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The thermal conductivity of meteorites: New measurements and analysis

Cited by 152 publications

References 17 publications

3D shape of asteroid (6) Hebe from VLT/SPHERE imaging: Implications for the origin of ordinary H chondrites

3D shape of asteroid (6) Hebe from VLT/SPHERE imaging: Implications for the origin of ordinary H chondrites

Early aqueous activity on the ordinary and carbonaceous chondrite parent bodies recorded by fayalite

Near-Earth asteroid (3200) Phaethon: Characterization of its orbit, spin state, and thermophysical parameters

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