Physical properties of M class asteroids

Belskaya, I. N.; Lagerkvist, C. I.

doi:10.1016/0032-0633(96)00021-9

Cited by 31 publications

(20 citation statements)

References 35 publications

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“…NIR spectroscopy (Birlan et al 2006) confirmed a similarity with CV-CO meteorites. Polarimetric observations supported the idea that the composition of Lutetia is similar to that of carbonaceous chondrite meteorites (Belskaya & Lagerkvist 1996). Magri et al (1999) inferred a low radar albedo for Lutetia that excluded the extensive exposure of bright pure metal on its surface.…”

Section: Introductionmentioning

confidence: 68%

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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Section: Introductionmentioning

confidence: 68%

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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“…Belskaya & Lagerkvist (1996) found that M-asteroids have a faster mean rotational period compared to S and C type asteroids. They interpreted this as an indication of an higher mean density that allows M-asteroids to survive energetic collisions without disruption, which increases their rotational angular momentum.…”

Section: Statistics [Here Table 6] [Here Figure 9]mentioning

confidence: 94%

Spectroscopic survey of M-type asteroids☆

Fornasier

Clark

Dotto

et al. 2010

Icarus

104

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M-type asteroids, as defined in the Tholen taxonomy (Tholen, 1984), are medium albedo bodies supposed to have a metallic composition and to be the progenitors both of differentiated iron-nickel meteorites and enstatite chondrites. We carried out a spectroscopic survey in the visible and near infrared wavelength range (0.4-2.5 µm) of 30 asteroids chosen from the population of asteroids initially classified as Tholen M-types, aiming to investigate their surface composition. The data were obtained during several observing runs during the years 2004-2007 at the TNG, NTT, and IRTF telescopes. We computed the spectral slopes in several wavelength ranges for each observed asteroid, and we searched for diagnostic spectral features. We confirm a large variety of spectral behaviors for these objects as their spectra are extended into the near-infrared, including the identification of weak absorption bands, mainly of the 0.9 µm band tentatively attributed to orthopyroxene, and of the 0.43 µm band that may be associated to chlorites and Mgrich serpentines or pyroxene minerals such us pigeonite or augite. A comparison with previously published data indicates that the surfaces of several asteroids belonging to the M-class may vary significantly.We attempt to constrain the asteroid surface compositions of our sample by looking for 1 Based on observations carried out at the European Southern Observatory (ESO), La Silla, Chile, ESO proposals 073.C-0622, 074.C-0049 and 078.C-0115 and at the Telescopio Nazionale Galileo, Canary Islands, Spain. Preprint submitted to IcarusJanuary 30, 2018 meteorite spectral analogues in the RELAB database and by modelling with geographical mixtures of selected meteorites/minerals. We confirm that iron meteorites, pallasites, and enstatite chondrites are the best matches to most objects in our sample, as suggested for M-type asteroids. For 22 Kalliope, we demonstrate that a syntetic mixture obtained enriching a pallasite meteorite with small amounts (1-2%) of silicates well reproduce the spectral behaviour including the observed 0.9 µm feature.The presence of subtle absorption features on several asteroids confirms that not all objects defined by the Tholen M-class have a pure metallic composition.A statistical analysis of spectral slope distribution versus orbital parameters shows that our sample originally defined as Tholen M-types tend to be dark in albedo and red in slope for increasing value of the semi-major axis. However, we note that our sample is statistically limited by our number of objects (30) and slightly varying results are found for different subsets. If confirmed, the albedo and slope trends could be due to a difference in composition of objects belonging to the outer main belt, or alternatively to a combination of surface composition, grain size and space weathering effects.

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“…Laboratory measurements of iron meteorites and enstatite chondrites with particle sizes smaller than 50 μm infer smaller inversion angles than measured for Lutetia's surface (Lupishko & Belskaya 1989). A CV3 type of carbonaceous chondrites was mentioned as the closest polarimetric analogue of Lutetia (Belskaya & Lagerkvist 1996). Figure 7 shows an updated relationship between P min and α inv for asteroids and meteorites.…”

Section: Polarimetrymentioning

confidence: 96%

“…On the basis of spectral and polarimetric observations, three types of meteorites are generally taken into consideration as possible analogues: iron meteorites (Bowell et al 1978;Dollfus et al 1979), enstatite chondrites (Chapman et al 1975;Vernazza et al 2009), and some types of carbonaceous chondrites, mainly CO3 or CV3 (Belskaya & Lagerkvist 1996;Birlan et al 2004;Barucci et al 2008;Lazzarin et al 2009). The main problem in spectral data interpretation is the featureless spectrum of Lutetia.…”

Section: Introductionmentioning

confidence: 99%

Puzzling asteroid 21 Lutetia: our knowledge prior to the Rosetta fly-by

Belskaya

Fornasier

Krugly

et al. 2010

A&A

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Aims. A wide observational campaign was carried out in [2004][2005][2006][2007][2008][2009] that aimed to complete the ground-based investigation of Lutetia prior to the Rosetta fly-by in July 2010. Methods. We obtained BVRI photometric and V-band polarimetric measurements over a wide range of phase angles, and visible and infrared spectra in the 0.4-2.4 μm range. We analyze them with previously published data to retrieve information about Lutetia's surface properties.Results. Values of lightcurve amplitudes, absolute magnitude, opposition effect, phase coefficient, and BVRI colors of Lutetia surface seen at near pole-on aspect are determined. We define more precisely parameters of polarization phase curve and show their distinct deviation from any other moderate-albedo asteroid. An indication of possible variations in both polarization and spectral data across the asteroid surface are found. To explain features found by different techniques, we propose that (i) Lutetia has a non-convex shape, probably due to a large crater, and heterogeneous surface properties probably related to surface morphology; (ii) at least part of the surface is covered by a fine-grained regolith of particle size smaller than 20 μm; (iii) the closest meteorite analogues of Lutetia's surface composition are particular types of carbonaceous chondrites, or Lutetia has specific surface composition that is not representative among studied meteorites.

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Physical properties of M class asteroids

Cited by 31 publications

References 35 publications

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

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

Spectroscopic survey of M-type asteroids☆

Puzzling asteroid 21 Lutetia: our knowledge prior to the Rosetta fly-by

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