Investigations of D-type asteroids

Lagerkvist, C.‐I.; Fitzsimmons, A.; Magnusson, P.; Williams, I. P.

doi:10.1093/mnras/260.3.679

Cited by 9 publications

(10 citation statements)

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“…The correlation seems not to be exclusive of the ACOs since it is also present in most of the other samples with the exception of Trojan asteroids, as all of them have similar semi-major axis. This indicates that objects farthest from the sun are reddest, as was already pointed out by diverse authors (Vilas & Smith 1985;Hartmann et al 1987;Lagerkvist et al 1993;. The NEO and non-NEO samples share the overall behavior of the total ACO sample, though with different degrees of reliability.…”

Section: Search For Correlationssupporting

confidence: 53%

“…This arises from the relationship between T and eccentricity through The correlation found between S V and semi-major axis was first suggested by Vilas & Smith (1985) and Harmann et al (1987) and strongly supported by Lagerkvist et al (1993) analyzing the spectra of a sample of D-type asteroids. On the other hand Carvano et al (2003) did not find any correlation, analyzing a larger sample of featureless spectra.…”

Section: Search For Correlationsmentioning

confidence: 79%

“…On the other hand Carvano et al (2003) did not find any correlation, analyzing a larger sample of featureless spectra. Nevertheless, their analysis was performed on a sample located mostly in the inner region of the asteroid belt, while our analysis, as well as Lagerkvist et al (1993) uses a sample of objects located mostly in the outer belt. Note that we have found the correlation not only for the ACOs but also for the extended sample, including objects from NEO orbits to Trojan asteroids.…”

Section: Search For Correlationsmentioning

confidence: 99%

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Spectral properties of asteroids in cometary orbits

Licandro¹,

Álvarez-Candal

León³

et al. 2008

A&A

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Aims.In this paper we analyze the spectra of a sample of asteroids in cometary orbits (ACOs) in order to understand the relationship between them, the Jupiter family comets (JFCs), and the outer main belt populations, such as Hilda, Trojan and Cybele asteroids. Methods. We obtained visible (0.55−0.90 µm) and/or near-infrared (0.8−2.3 µm) spectra of 24 ACOs using 3 telescopes at the "Roque de los Muchachos" Observatory (La Palma, Spain). Using this data, we derived the taxonomic classification of the asteroids. As most ACOs present featureless spectra (B-, C-, P-, D-type) we also derived their spectral gradient (S ). Considering also published spectra of ACOs we correlated S with orbital and dynamical parameters and obtained the cumulative distribution of S , and compare it with that of other related populations.Results. We present visible and/or near infrared spectra of 24 ACOs, most of them (21) presenting featureless spectra. After including the spectra of other ACOs already published, we analyzed a total of 41 objects, 34 of them having featureless spectra like the spectra of comet nuclei and outer main-belt asteroids. We also noticed a significant difference in the taxonomic distribution of the ACOs in Near-Earth orbits (q < 1.3 AU) and those that are not (q > 1.3 AU), indicative of different source/transport mechanisms. About 35% of the ACOs in the NEO population analyzed have spectra that present the typical silicate absorption bands at 1 and 2 µm (S-and V-type), while only 1 of the 24 ACOs in the non-NEO population (about 4%) is S-type and the other 23 have a featureless spectrum. Thus the NEO sub-population of ACOs is composed of a significant fraction of asteroids scattered from the inner main-belt. We didn't find any subtle features in the 0.5−2.0 µm spectral region of featureless ACOs that can be used to discriminate wheather an ACO comes from a cometary or an asteroidal origin. The analysis of the spectral gradient shows that ACOs present an interesting, and significant, anti-correlation between the Tisserand parameter and the "spectral gradient", meaning that the reddest objects have the lower Tisserand parameter (i.e., higher chance of a cometary origin). Finally, we obtained the S cumulative distribution for ACOs. This distribution is "bluer" than that of comet nuclei, Damocloids and outer main-belt population of asteroids, indicative of a significant "contamination" of asteroids scattered from the inner main-belt.

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Section: Search For Correlationssupporting

confidence: 53%

Section: Search For Correlationsmentioning

confidence: 79%

Section: Search For Correlationsmentioning

confidence: 99%

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Spectral properties of asteroids in cometary orbits

Licandro¹,

Álvarez-Candal

León³

et al. 2008

A&A

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“…In fact, it has long been suggested that objects with featureless and steep spectra exist across a larger portion of the main belt, but their exact nature and relation to their more canonical twins in the Hilda and Trojans regions was discussed (see, e.g.,Lagerkvist et al 1993;Fitzsimmons et al 1994;Carvano et al 2003). This was also because these earlier works lacked substantiation by the absence of spectral information extending to the near-infrared part of the spectrum.…”

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confidence: 99%

Capture of Trans-Neptunian Planetesimals in the Main Asteroid Belt

2016

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The orbital evolution of the giant planets after nebular gas was eliminated from the Solar System but before the planets reached their final configuration was driven by interactions with a vast sea of leftover planetesimals. Several variants of planetary migration with this kind of system architecture have been proposed. Here, we focus on a highly successful case, which assumes that there were once five planets in the outer Solar System in a stable configuration: Jupiter, Saturn, Uranus, Neptune, and a Neptune-like body. Beyond these planets existed a primordial disk containing thousands of Pluto-sized bodies, ∼50 million D > 100 km bodies, and a multitude of smaller bodies. This system eventually went through a dynamical instability that scattered the planetesimals and allowed the planets to encounter one another. The extra Neptune-like body was ejected via a Jupiter encounter, but not before it helped to populate stable niches with disk planetesimals across the Solar System. Here, we investigate how interactions between the fifth giant planet, Jupiter, and disk planetesimals helped to capture disk planetesimals into both the asteroid belt and first-order mean-motion resonances with Jupiter. Using numerical simulations, we find that our model produces the right proportion of P-and D-type asteroids in the inner, central, and outer main belt, while also populating the Hilda and Thule regions in Jupiter's 3/2 and 4/3 resonances. Moreover, the largest observed P/D types in each sub-population are an excellent fit to our captured population results (within uncertainties). The model produces a factor of ∼10 overabundance of diameter D > 10 km P/D types in the main belt, but this mismatch can likely be explained by various removal mechanisms (e.g., collision evolution over 4 Gyr, dynamical losses via Yarkovsky thermal forces over 4 Gyr, thermal destruction of the planetesimals en route to the inner solar system). Overall, our instability model provides a more satisfying match to constraints than that of Levison et al., and it provides us with strong supporting evidence that the five giant planet instability model is reasonable. Our results lead us to predict that D-type asteroids found in the near-Earth object population on low delta-V orbits with Earth are the surviving relics from the same source population that now make up the Kuiper Belt, the irregular satellites, and the Jupiter Trojans. The singular Tagish Lake meteorite, a primitive sample unlike other carbonaceous chondrite meteorites, is likely a fragment from a D-type asteroid implanted into the inner main belt. This would effectively make it the first known hand sample with the same composition as Kuiper Belt objects.

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“…Differences among D-type asteroids have been investigated by several authors, like Lagerkvist et al (1993) who reported a clear correlation between the color index and the heliocentric distance, and Carvano et al (2003) who noticed that inner main-belt D-types have more concave spectral shapes and higher albedos than those in the outer main-belt. In this work we study the spectra of 100 D-type asteroids, obtained from the public spectroscopic surveys SMASSII (Bus & Binzel 2002), S3OS2 (Lazzaro et al 2004), and from the work of Fornasier et al (2004), where it is possible to find the details of the respective observations.…”

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confidence: 99%

Searching for minor absorptions on D-type asteroids

Mothé-Diniz¹

2009

Proc. IAU

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Abstract. Preferably located in the outer main belt, D-type asteroids experienced less heating and represent an important population for studies on the origin and evolution of the asteroid belt, as well as the relations between asteroidal and cometary bodies. Their surface mineralogy is currently related to a mixture of organics, anhydrous silicates, opaque material and ice. However, like other taxonomic classes, a large spectral diversity can be seen among D-type objects. We use the Visible spectra of 100 D-type objects available in the literature to search for minor absorptions in those objects. The presence of minor absorptions around 0.6 and 0.8 microns is reported for a large number of objects in the sample. The presence of such bands is not related to the heliocentric distance of the objects, since the absorptions can be seen in the whole main belt, up to the the Trojans region.

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Investigations of D-type asteroids

Cited by 9 publications

References 0 publications

Spectral properties of asteroids in cometary orbits

Spectral properties of asteroids in cometary orbits

Capture of Trans-Neptunian Planetesimals in the Main Asteroid Belt

Searching for minor absorptions on D-type asteroids

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