Identification of Magnetite in B-Type Asteroids

Yang, Bin; Jewitt, David

doi:10.1088/0004-6256/140/3/692

Cited by 40 publications

(19 citation statements)

References 70 publications

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“…Based on the spectral effects of carbons shown here, we suggest that the B-class asteroid spectra presented in this report (Figure 1) (in particular, 702 Alauda and 704 Interamnia), with less-steep UV spectral slopes, could be controlled by carbonized materials. This is an alternative scenario to the idea posed by Yang and Jewitt (2010) that magnetite in B-class asteroids is responsible for the blue visible slope, with implications for aqueous alteration of these asteroids. Indeed, carbon as an explanation for the relatively blue slopes would be more consistent with the idea that these asteroids do not exhibit 0.7-μm absorption features.…”

Section: Discussion: Implications For Other Asteroidsmentioning

confidence: 80%

C‐Complex Asteroids: UV‐Visible Spectral Characteristics and Implications for Space Weathering Effects

Hendrix

Vilas

2019

Geophysical Research Letters

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Space weathering effects on the rocky S-class asteroids are well understood. However, on the low-albedo C-complex asteroids, such as spacecraft targets Bennu and Ryugu, the situation is more complicated, especially due to a lack of spectral features throughout the visible-near infrared spectral region. Here we show, through a combination of observational data and laboratory data of carbonaceous chondrites, phyllosilicates, and mixtures, that the UV-visible spectral region is a diagnostic regime for studying space weathering effects on C-complex asteroids. We show that space-weathering-produced opaque constituents, such as graphitized carbons, darken mixtures with phyllosilicates and produce a bluing the UV-visible spectrum, consistent with what is seen on the asteroids compared with carbonaceous chondrites. Furthermore, we demonstrate that the UV upturns in the spectra of Bennu and Ryugu are consistent with the presence of graphitized carbon on those surfaces, the result of surface processing. Plain Language SummaryWe suggest that the relatively weak UV absorptions of C-complex asteroids compared with carbonaceous chondrite meteorites could be due to the increased presence of carbonized species on the asteroid surfaces, the result of space weathering processes. In fact, carbonized materials could be the source of the UV-visible spectra of Ryugu and Bennu, which appear to show UV upturns rather than UV absorptions. Though iron-rich and carbon-rich opaques have similar spectral effects in the UV-VIS, many laboratory experiments indicate that carbonaceous materials are the products of space weathering processes and thus carbonaceous materials could dominate spectral trends. Furthermore, we show that carbons may exhibit spectral features that change with processing and thus can help us to understand exposure age of some low-albedo targets.

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Section: Discussion: Implications For Other Asteroidsmentioning

confidence: 80%

C‐Complex Asteroids: UV‐Visible Spectral Characteristics and Implications for Space Weathering Effects

Hendrix

Vilas

2019

Geophysical Research Letters

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“…Other products of aqueous alteration, such as magnetite, have been detected on asteroids (e.g. Yang and Jewitt, 2010), so it is possible that the absorptions observed in the spectrum of Themis are due to similar materials other than goethite. If the H 2 O ice is thermally decoupled from the regolith (i.e.…”

Section: Discussionmentioning

confidence: 99%

Observational constraints on water sublimation from 24 Themis and 1 Ceres

McKay¹,

Bodewits

2017

Icarus

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Recent observations have suggested that there is water ice present on the surfaces of 24 Themis and 1 Ceres. We present upper limits on the H 2 O production rate on these bodies derived using a search for [O I]6300Å emission.For Themis, the water production is less than 4.5 × 10 27 mol s −1 , while for Ceres our derived upper limit is 4.6 × 10 28 mol s −1 . The derived limits imply a very low fraction of the surface area of each asteroid is active (< 2 × 10 −4 ), though this estimate varies by as much as an order of magnitude depending on thermal properties of the surface. This is much lower than seen for comets, which have active areas of 10 −2 -10 −1 . We discuss possible implications for our findings on the nature of water ice on Themis and Ceres.

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“…The size and shape of the minimum do not appear to be related to the steepness of the visual or red slopes. The broad minimum around 1000 nm, seen in some B‐class spectra and in the spectrum of 704 Interamnia, was recently ascribed to magnetite by Yang and Jewitt (2010).…”

Section: Main Belt Asteroids Similar To 2008 Tc3mentioning

confidence: 94%

Almahata Sitta (=asteroid 2008 TC₃) and the search for the ureilite parent body

Jenniskens

Vaubaillon

Binzel

et al. 2010

Meteorit & Planetary Scien

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Abstract-This article explores what the recovery of 2008 TC 3 in the form of the Almahata Sitta meteorites may tell us about the source region of ureilites in the main asteroid belt. An investigation is made into what is known about asteroids with roughly the same spectroscopic signature as 2008 TC 3 . A population of low-inclination near-Earth asteroids is identified with spectra similar to 2008 TC 3 . Five asteroid families in the Main Belt, as well as a population of ungrouped asteroids scattered in the inner and central belts, are identified as possible source regions for this near-Earth population and 2008 TC 3 . Three of the families are ruled out on dynamical and spectroscopic grounds. New near-infrared spectra of 142 Polana and 1726 Hoffmeister, lead objects in the two other families, also show a poor match to Almahata Sitta. Thus, there are no Main Belt spectral analogs to Almahata Sitta currently known. Space weathering effects on ureilitic materials have not been investigated, so that it is unclear how the spectrum of the Main Belt progenitor may look different from the spectra of 2008 TC 3 and the Almahata Sitta meteorites. Dynamical arguments are discussed, as well as ureilite petrogenesis and parent body evolution models, but these considerations do not conclusively point to a source region either, other than that 2008 TC 3 probably originated in the inner asteroid belt.

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Identification of Magnetite in B-Type Asteroids

Cited by 40 publications

References 70 publications

C‐Complex Asteroids: UV‐Visible Spectral Characteristics and Implications for Space Weathering Effects

C‐Complex Asteroids: UV‐Visible Spectral Characteristics and Implications for Space Weathering Effects

Observational constraints on water sublimation from 24 Themis and 1 Ceres

Almahata Sitta (=asteroid 2008 TC₃) and the search for the ureilite parent body

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Identification of Magnetite in B-Type Asteroids

Cited by 40 publications

References 70 publications

C‐Complex Asteroids: UV‐Visible Spectral Characteristics and Implications for Space Weathering Effects

C‐Complex Asteroids: UV‐Visible Spectral Characteristics and Implications for Space Weathering Effects

Observational constraints on water sublimation from 24 Themis and 1 Ceres

Almahata Sitta (=asteroid 2008 TC3) and the search for the ureilite parent body

Contact Info

Product

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Almahata Sitta (=asteroid 2008 TC₃) and the search for the ureilite parent body