Small Main-Belt Asteroid Spectroscopic Survey in the Near-Infrared

Burbine, T. H.; Binzel, Richard P.

doi:10.1006/icar.2002.6902

Cited by 112 publications

(73 citation statements)

References 42 publications

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“…The diameter estimated from the absolute magnitude (13.18), assuming an albedo value of 0.2, is between 8-10 km. Comparing the spectral behavior of Litva with that of 9 A-type asteroids reported by Burbine & Binzel (2002), it appears that Litva has a higher abundance of olivine as compared to other small-sized A-type asteroids.…”

Section: Litvamentioning

confidence: 76%

Visible and near infrared spectroscopic investigation of E-type asteroids, including 2867 Steins, a target of the Rosetta mission☆

Fornasier

Migliorini

Dotto

et al. 2008

Icarus

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. Visible and near infrared spectroscopic investigation of E-type asteroids, including 2867 Steins, a target of the Rosetta mission. Icarus, Elsevier, 2009, 196 (1) This is a PDF file of an unedited manuscript that has been accepted for publication. As a service to our customers we are providing this early version of the manuscript. The manuscript will undergo copyediting, typesetting, and review of the resulting proof before it is published in its final form. Please note that during the production process errors may be discovered which could affect the content, and all legal disclaimers that apply to the journal pertain. AbstractWe present the results of a visible spectroscopic and photometric survey of igneous asteroids belonging to the small and intriguing Eclass, including 2867 Steins, a target of the Rosetta mission. The survey was carried out at the 3.5m Telescopio Nazionale Galileo (TNG), and at the 3.5m New Technology Telescope (NTT) of the European Southern Observatory. We obtained new visible spectra for eighteen E-type asteroids, and near infrared spectra for eight of them. We confirm the presence of three different mineralogies in the small E-type populations. We classify each object in the E To fully investigate the E-type population, we enlarged our sample including 6 E-type asteroids spectra available in literature, resulting in a total sample of 21 objects. The analysis of the spectral slope for the 3 different E-type subgroups versus the orbital elements show that E[III] members have the lowest mean spectral slope value inside the whole sample, and that they are located between 2.2-2.7 AU in low inclination orbits. E[II] members has the highest spectral slope inside the sample, half of them are located in the Hungaria region, 2 are NEA and 2 (64 Angelina and 2867 Steins), are in the main belt. A similar distribution is found for the 5 featureless E[I] members, located mainly in the Hungaria region (3 members), one in the middle main belt while one is a NEA (2004 VD17). Finally, for the five E-type asteroids observed both in the visible and near infrared range, plus 2867 Steins, we attempt to model their surface composition using linear geographycal mixtures of no more than 3 components, selected from aubrite meteorites and correlated minerals. In particular we suggest that the aubrite Peña Blanca might have the E[III] asteroid 317 Roxane as parent body, and that the aubrite ALH78113 might be related to the E[II] subgroup asteroids.

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Section: Litvamentioning

confidence: 76%

Visible and near infrared spectroscopic investigation of E-type asteroids, including 2867 Steins, a target of the Rosetta mission☆

Fornasier

Migliorini

Dotto

et al. 2008

Icarus

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“…However, ordinary chondrites and HED achondrites exhibit deep absorption bands of mafic silicates in the near-infrared, while Lutetia is relatively featureless in that spectral range (Howell et al 1994;Burbine & Binzel 2002;Birlan et al 2004Birlan et al , 2006Nedelcu et al 2007). Among meteorites with relatively featureless NIR spectra, a broad inflection mentioned above is present in the spectra of some chondrites of CR clan (including CH) and ureilites.…”

Section: Observations Data Reduction and Discussionmentioning

confidence: 99%

“…Lazzaro et al (2004) also determined an X-classification for Lutetia. Howell et al (1994) and Burbine & Binzel (2002) observed Lutetia in the near-infrared and found that it has an unusual flat spectrum compared to other M-type asteroids.…”

Section: Introductionmentioning

confidence: 99%

New visible spectra and mineralogical assessment of (21) Lutetia, a target of the Rosetta mission

Lazzarin

Marchi

Moroz

et al. 2009

A&A

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The Rosetta spacecraft, launched on March 2nd 2004, in the course of its journey to the comet 67P/Churyumov-Gerasimenko (encounter foreseen in 2014), will fly past two asteroids: (2867) Steins and (21) Lutetia. On September 5th 2008 (2867) Steins was encountered. In this paper, we present two visible spectra of (21) Lutetia of different spectral resolutions covering the spectral ranges where possible absorption bands were previously revealed by Lazzarin and collaborators. We confirm detection of a broad complex feature between 0.45 and 0.55 μm and two narrower features around 0.47 and 0.52 μm. We discuss possible assignments of these bands and suggest that they might originate from electronic transitions in pyroxenes, although unambiguous identification is difficult and the published thermal infrared (TIR) spectrum of (21) Lutetia suggests that pyroxene cannot be the dominant silicate component at its surface. Furthermore, we discuss the published spectra of (21) Lutetia in the range from near-UV to thermal infrared. We conclude that carbonaceous meteorites (chondrites and achondrites) appear to be the closest meteorite analogues of (21) Lutetia, based on the observed spectral features. Among these meteorites, metal-rich carbonaceous chondrites seem to be the most plausible analogue materials.

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“…In this regard, the most fundamental distinction would be between objects of classes belonging to the S-complex (Bus & Binzel 2002) and those classified in the C-or X-complexes (Bus & Binzel 2002), which also have low geometric albedos. The S-complex asteroids, whose spectra is dominated in the visible by olivine/pyroxene bands, in general should have mineralogies compatible with the anhydrous and poorly hydrated chondrites, i.e., OCs and CO/CVs, as well as several products of differentiation (Britt et al 1992;Burbine & Binzel 2002;Mothe-Diniz et al 2008). The best mineralogical analogues for objects with low albedo classified in the C-/X-complexes are the hydrated carbonaceous chondrites CM and CI (Vilas & Gaffey 1989;Carvano et al 2003) Members of these complexes with higher albedos, on the other hand, can be compatible with differentiation products as enstatite achondrites and metallic meteorites, as well as with enstatite chondrites.…”

Section: Distribution Of Taxonomiesmentioning

confidence: 99%

On the current distribution of main belt objects: Constraints for evolutionary models

Michtchenko

Lazzaro

Carvano

2016

A&A

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Context. It is widely accepted that the current distribution of material in the main asteroidal belt (MB) is a product of the evolutionary history of the solar system during its whole lifetime of ∼4.5 billions of years and is, consequently, a major witness of the diverse stages of this evolution. Aims. The purpose of this paper is twofold: first, we study the principal aspects of the distribution of the asteroids in proper element space, mass, and, physical composition for a complete picture of the current MB. Second, we analyze if and how these current distributions can be explained by the long-lasting dynamical effects of the planets on this region of the solar system. Methods. We studied the distribution in the proper element space for the sample that consists of about 350 000 objects whose proper orbital elements are available from the database AstDyS. We studied the distribution in size and physical composition using the most recent and large available datasets. We constructed the dynamical portrait of the MB in form of the dynamical and averaged maps via the spectral analysis method. Results. The main properties of the current distributions of MB objects are identified. A comparison of the distributions of real objects with dynamical maps allows us to detect principal mechanisms of the diffusive transportation of the objects. These mechanisms are related to mean-motion resonances (MMRs) and secular resonances (SRs), overlaying with the slow dissipative Yarkovsky/Yorp drift. Conclusions. We identify the most relevant distributions of the material in the MB and show that many of the current features of the MB can be explained by the interplay of diverse dynamical mechanisms due to the planetary perturbations over 4 Gyr with nongravitational effects, without the need of 'catastrophic' events or 'ad hoc' migration mechanisms during the early stages of the solar system. In this sense, the obtained distributions can provide relevant constraints for modeling the origin and evolution of the MB.

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Small Main-Belt Asteroid Spectroscopic Survey in the Near-Infrared

Cited by 112 publications

References 42 publications

Visible and near infrared spectroscopic investigation of E-type asteroids, including 2867 Steins, a target of the Rosetta mission☆

Visible and near infrared spectroscopic investigation of E-type asteroids, including 2867 Steins, a target of the Rosetta mission☆

New visible spectra and mineralogical assessment of (21) Lutetia, a target of the Rosetta mission

On the current distribution of main belt objects: Constraints for evolutionary models

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