Water and the thermal evolution of carbonaceous chondrite parent bodies

Grimm, R. E.; McSween, H. Y.

doi:10.1016/0019-1035(89)90038-9

Cited by 298 publications

(256 citation statements)

References 57 publications

Supporting

Mentioning

243

Contrasting

Unclassified

Order By: Relevance

“…Initially parent bodies beyond the snow line are believed to be mixtures of water ice and silicates, which are then heated due to the radioactive decay of 26 Al within 1-2 million years after nebular collapse (Krot et al 2006). Grimm & McSween (1989) find that once the water is liquid, it is consumed by hydration reactions, preferentially in the interior (Cohen & Coker 2000;Wilson et al 1999), possibly leaving ice in the outer layers. In the inner asteroid belt, it is likely that most of that water has been converted in hydrated material observed on S-type asteroids (Rivkin et al 2002).…”

Section: Introductionmentioning

confidence: 91%

P/2010 a2 Linear

Hainaut

Kleyna

Sarid

et al. 2012

A&A

View full text Add to dashboard Cite

Comet P/2010 A2 LINEAR is an object on an asteroidal orbit within the inner main belt, therefore a good candidate for membership with the main belt comet family. It was observed with several telescopes (ESO New Technology Telescope, La Silla, Chile; Gemini North, Mauna Kea, Hawaii; University of Hawaii 2.2 m, Mauna Kea, Hawaii) from 14 Jan. until 19 Feb. 2010 in order to characterize and monitor it and its very unusual dust tail, which appears almost fully detached from the nucleus; the head of the tail includes two narrow arcs forming a cross. No evolution was observed during the span of the observations. Observations obtained during the Earth orbital plane crossing allowed an examination of the out-of-plane 3D structure of the tail. The immediate surroundings of the nucleus were found dust-free, which allowed an estimate of the nucleus radius of 80-90 m, assuming an albedo p = 0.11 and a phase correction with G = 0.15 (values typical for S-type asteroids). A model of the thermal evolution indicates that such a small nucleus could not maintain any ice content for more than a few million years on its current orbit, ruling out ice sublimation dust ejection mechanism. Rotational spin-up and electrostatic dust levitations were also rejected, leaving an impact with a smaller body as the favoured hypothesis. This is further supported by the analysis of the tail structure. Finston-Probstein dynamical dust modelling indicates the tail was produced by a single burst of dust emission. More advanced models (described in detail in a companion paper), independently indicate that this burst populated a hollow cone with a half-opening angle α ∼ 40 • and with an ejection velocity v max ∼ 0.2 m s −1 , where the small dust grains fill the observed tail, while the arcs are foreshortened sections of the burst cone. The dust grains in the tail are measured to have radii between a = 1-20 mm, with a differential size distribution proportional to a −3.44±0.08 . The dust contained in the tail is estimated to at least 8 × 10 8 kg, which would form a sphere of 40 m radius (with a density ρ = 3000 kg m −3 and an albedo p = 0.11 typical of S-type asteroids). Analysing these results in the framework of crater physics, we conclude that a gravity-controlled crater would have grown up to ∼100 m radius, i.e. comparable to the size of the body. The non-disruption of the body suggest this was an oblique impact.

show abstract

Section: Introductionmentioning

confidence: 91%

P/2010 a2 Linear

Hainaut

Kleyna

Sarid

et al. 2012

A&A

View full text Add to dashboard Cite

show abstract

“…The source of sublimation in these MBCs is attributed to water ice buried beneath a layer of regolith several meters thick (Schorghofer 2008;Prialnik & Rosenberg 2009). Thermal evolution models suggest the Themis/Beagle parent body was likely differentiated, with aqueous alteration taking place predominantly in the core, thus allowing the preservation of an icy shell near the surface (Castillo-Rogez & Schmidt 2010;Grimm & McSween 1989;Cohen & Coker 2000).…”

Section: Aqueous Alteration In the Themis Parent Bodymentioning

confidence: 99%

Space weathering trends among carbonaceous asteroids

Kaluna

Masiero

Meech

2016

Icarus

View full text Add to dashboard Cite

We present visible spectroscopic and albedo data of the 2.3 Gyr old Themis family and the <10 Myr old Beagle sub-family. The slope and albedo variations between these two families indicate C-complex asteroids become redder and darker in response to space weathering. Our observations of Themis family members confirm previously observed trends where phyllosilicate absorption features are less common among small diameter objects. Similar trends in the albedos of large (>15 km) and small (≤15 km) Themis members suggest these phyllosilicate feature and albedo trends result from regolith variations as a function of diameter. Observations of the Beagle asteroids show a small, but notable fraction of members with phyllosilicate features. The presence of phyllosilicates and the dynamical association of the main-belt comet 133P/Elst-Pizarro with the Beagle family imply the Beagle parent body was a heterogenous mixture of ice and aqueously altered minerals.Subject headings: main belt asteroids, carbonaceous asteroids, space weathering

show abstract

“…We consider the static water model 20,23 here, although the fluid flow model has been investigated in some previous works [24][25][26][27] . The thermal history is modelled using a onedimensional heat conduction equation in radial form.…”

Section: − +mentioning

confidence: 99%

Evidence for the late formation of hydrous asteroids from young meteoritic carbonates

et al. 2012

View full text Add to dashboard Cite

The accretion of small bodies in the solar system is a fundamental process that was followed by planet formation. Chronological information of meteorites can constrain when asteroids formed. secondary carbonates show extremely old 53 mn-53 Cr radiometric ages, indicating that some hydrous asteroids accreted rapidly. However, previous studies have failed to define accurate mn/Cr ratios; hence, these old ages could be artefacts. Here we develop a new method for accurate mn/Cr determination, and report a reliable age of 4,563.4+0.4/-0.5 million years ago for carbonates in carbonaceous chondrites. We find that these carbonates have identical ages, which are younger than those previously estimated. This result suggests the late onset of aqueous activities in the solar system. The young carbonate age cannot be explained if the parent asteroid accreted within 3 million years after the birth of the solar system. Thus, we conclude that hydrous asteroids accreted later than differentiated and metamorphosed asteroids.

show abstract

Water and the thermal evolution of carbonaceous chondrite parent bodies

Cited by 298 publications

References 57 publications

P/2010 a2 Linear

P/2010 a2 Linear

Space weathering trends among carbonaceous asteroids

Evidence for the late formation of hydrous asteroids from young meteoritic carbonates

Contact Info

Product

Resources

About