Detection of ice and organics on an asteroidal surface

Rivkin, A. S.; Emery, Joshua P.

doi:10.1038/nature09028

Cited by 326 publications

(291 citation statements)

References 12 publications

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“…The first is that heterogeneity may represent non-uniform alteration of the Themis/Beagle parent body. Conversely, Rivkin & Emery (2010) and Campins et al (2010) have potentially detected water ice features on the largest member of the family, 24 Themis. Castillo-Rogez & Schmidt (2010) suggest 24 Themis is the remnant silicate rich core onto which components of its icy crust may have reaccreted following the collisional disruption of the parent body.…”

Section: Aqueous Alteration In the Themis Parent Bodymentioning

confidence: 99%

Space weathering trends among carbonaceous asteroids

Kaluna

Masiero

Meech

2016

Icarus

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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

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Section: Aqueous Alteration In the Themis Parent Bodymentioning

confidence: 99%

Space weathering trends among carbonaceous asteroids

Kaluna

Masiero

Meech

2016

Icarus

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“…In the ∼ 100 km diameter range, asteroid (24) Themis bears some significance in the debate of whether ice can originate from and survive in the Main Belt (MB), as water ice may have been detected at its surface (Campins et al 2010;Rivkin and Emery 2010) via an absorption feature near 3 µm. We note that Themis was not found to be active by Jewitt and Guilbert-Lepoutre (2012), who suggested that if indeed present at its surface, water ice should be relatively clean and confined to a limited spatial extent, which was then confirmed by McKay et al (2017).…”

Section: Evidence For Water In Asteroidsmentioning

confidence: 99%

The Main Belt Comets and ice in the Solar System

Snodgrass

Agarwal

Combi

et al. 2017

Astron Astrophys Rev

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We review the evidence for buried ice in the asteroid belt; specifically the questions around the so-called Main Belt Comets (MBCs). We summarise the evidence for water throughout the Solar System, and describe the various methods for detecting it, including remote sensing from ultraviolet to radio wavelengths. We review progress in the first decade of study of MBCs, including observations, modelling of ice survival, and discussion on their origins. We then look at which methods will likely be most effective for further progress, including the key challenge of direct detection of (escaping) water in these bodies.

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“…Absorption features are detected in the spectra of many C-types (Lebofsky 1980;Jones et al 1990;Rivkin et al 2002), consistent with the presence of a significant fraction of hydrated minerals. Water ice and organics were recently detected using 2-4 μm spectroscopy in the surface of C-type asteroid (24) Themis (hereafter Themis, Campins et al 2010;Rivkin & Emery 2010), an asteroid in the edge of the main belt, with a = 3.13 AU. Themis is the largest member of a collisional family that has 2 members that presented comet-like activity according to Hsieh & Jewitt (2006).…”

Section: Introductionmentioning

confidence: 99%

(65) Cybele: detection of small silicate grains, water-ice, and organics

Licandro

Campins

Kelley

et al. 2010

A&A

109

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Context. (65) Cybele is the most representative member of a population of primitive asteroids in the outer edge of the main belt, the Cybele asteroids. Recent dynamical models suggest that a significant fraction of them originated in the primordial transneptunian disk, so the study of the physical properties of these asteroids is potentially a useful test of these models. Aims. Our aim is to obtain information on the surface composition of this asteroid. In particular we want to obtain information on the composition and properties of the regolith and the possible presence of ices and organic materials. Methods. We present 2-4 μm and 5-14 μm spectroscopy of (65) Cybele obtained with the NASA IRTF telescope and Spitzer Space Telescope respectively. We compare the results with spectra of Trojan asteroids and asteroid (24) Themis. We analyze the 2-4 μm spectrum using scattering models and we apply thermal models to the 5-14 μm data. Results. The 2-4 μm spectrum of (65) Cybele presents an absorption band centered at ∼3.1 μm and more weaker bands in the 3.2-3.6 μm region, very similar to those observed in (24) Themis. No hydrated silicates are detected. From the spectrum in the 5-14 μm region an effective diameter D = 290 ± 5 km, a beaming paramete η = 0.967 ± 0.014, and a geometric visible albedo p V = 0.05 ± 0.01 are derived using the NEATM thermal model. The emisivity spectrum in the 5-14 μm range exhibits an emission plateau at about 9 to 12 μm with an spectral contrast of ∼5%. This emission is similar to that of Trojan asteroids and active comets and may be due to small silicate grains being imbedded in a relatively transparent matrix, or to a very under-dense (fairy-castle) surface structure. The lower amplitude of the silicate emission in Cybele's spectrum with respect to that of Trojan asteroids could be attributed to larger dust particles and/or a slightly denser structure. Conclusions. The surface of (65) Cybele is covered by a fine anhydrous silicate grains mantle, with a small amount of water ice and complex organic solids. This is similar to comet surface where non-equilibrium phases coexist. The presence of water-ice and anhydrous silicates is indicative that hydration did not happened or is incomplete, suggesting that the temperatures were always sufficiently low.

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Detection of ice and organics on an asteroidal surface

Cited by 326 publications

References 12 publications

Space weathering trends among carbonaceous asteroids

Space weathering trends among carbonaceous asteroids

The Main Belt Comets and ice in the Solar System

(65) Cybele: detection of small silicate grains, water-ice, and organics

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