V-type asteroids in the middle main belt

Roig, F.; Nesvorný, David; Gil-Hutton, R.; Lazzaro, D.

doi:10.1016/j.icarus.2007.10.004

Cited by 68 publications

(92 citation statements)

References 36 publications

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“…The V class characteristic spectrum is distinctive by having the deepest 1 μm band among observed asteroid spectra. This class is firmly associated with HED meteorites (McCord et al 1970), and is observed mostly in and around the Vesta family Burbine et al 2001;Florczak et al 2002;Alvarez-Candal et al 2006) in the inner main belt, with a few observed in the intermediate (Binzel et al 2006;Roig et al 2008;Moskovitz et al 2008;Nesvorný et al 2008) and outer belt (Lazzaro et al 2000;Duffard & Roig 2009). The O and Q classes are characterized by a not very deep 1 μm band and by a flatter spectrum shortwards the i band than the V class (with the Q class being more reddened in the region than the O class).…”

Section: Definition Of the Classesmentioning

confidence: 86%

SDSS-based taxonomic classification and orbital distribution of main belt asteroids

Carvano

Hasselmann

Lazzaro

et al. 2010

A&A

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Aims. The present paper aims to derive a new classification scheme for SDSS MOC asteroid colors that is compatible with previous taxonomies based on spectroscopic data. The distribution of these can give important clues to the formation and evolution of this region of the Solar System, as well as to locate candidates with mineralogically interesting spectra for detailed observations. Methods. The methodology is based on the large database SDSS MOC4. Templates of the main taxonomic classes are derived and then used to classify the asteroid observations in the SDSS MOC4. The derived taxonomic scheme is compatible with the Bus taxonomy and is suitable to the peculiarities of the SDSS observations, in particular, the low spectral resolution. Results. Density maps of the seven classes defined by the method reproduce classical results for the background which is mainly dominated by the S p class in the inner belt and by the X p and the C p classes beyond 2.8 AU. It also shows new structures, such as the fact that the X p and C p seem evenly distributed in the inner belt while in the outer belt the S p class increase in density only at the location of asteroid families. Although their overall distribution is similar, the X p class seems less frequently associated with large families than do the C p class asteroids. Although only clustering around the Vesta family, the V p class asteroidsnappear scattered all around the main belt. Besides the lack satisfactory explanations of most of the highlighted features, they may provide strong constraints on the models of the formation and evolution of the Solar System.

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Section: Definition Of the Classesmentioning

confidence: 86%

SDSS-based taxonomic classification and orbital distribution of main belt asteroids

Carvano

Hasselmann

Lazzaro

et al. 2010

A&A

Self Cite

163

254

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“…Although some of them can be directly linked to (4) Vesta, forming its dynamical family, others do not appear to have a clear dynamical link, suggesting, thus, the existence of other basaltic parent bodies. In particular, the discovery of small basaltic asteroids in the outer and intermediate main belt (Lazzaro et al 2000;Binzel et al 2006;Hammergren et al 2006;Moskovitz et al 2008;Roig et al 2008;Duffard & Roig 2009), as well as in the inner belt, but far away from the dynamical limits of the Vesta family (e.g. Xu et al 1995;Duffard et al 2004;Alvarez-Candal et al 2006), confirms that several differentiated parent bodies must have formed and proves that some of their basaltic material has survived over the life of the solar system.…”

Section: Introductionmentioning

confidence: 94%

Spectral and mineralogical characterization of inner main-belt V-type asteroids

Sanctis

Migliorini

Jasmin

et al. 2011

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Context. V-type asteroids in the inner main belt are thought to be genetically related to (4) Vesta as collisional fragments. We investigate their relationship with Vesta observing putative V-type asteroids. Aims. The aim of this work is to observe candidate V-type asteroids, selected in different regions of the inner main belt, to characterize them and hence better understand their relationship with (4) Vesta. Methods. We present new NIR reflectance spectra of 18 V-type candidate asteroids, selected from datasets of possible V-type asteroids. The data were obtained at the 3.6 m Telescopio Nazionale Galileo, covering the spectral range 0.7 to 2.5 μm. We derive spectral parameters from NIR spectra to infer mineralogical information of the observed asteroids. The spectra of these asteroids are examined and compared to those of Howardite-Eucrite-Diogenite meteorites (HED), of which (4) Vesta is believed to be the parent body, and other V-type asteroids observed during previous campaigns. To enlarge the data set and increase the statistical significance of the analysis, we included the data presented in our previous article, obtaining a final data set of 41 V-type asteroids. Results. The V-type asteroids examined here show a higher variability of band parameters with respect to HEDs values, as for (4) Vesta. This result indicates that (4) Vesta and V-type asteroids have mineralogies that are not completely represented in the HEDs collection.Conclusions. An important finding is that some of the observed asteroids show spectral characteristics similar to diogenites, a result that may have relevant implications on their origin. Moreover, most of the diogenitic asteroids are not members of the Vesta classical family.

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“…This hypothesis is slightly problematic as de Elía & Brunini (2007) have actually found that mixing should be minimal among zones of the main asteroid belt delineated by the strongly chaotic 3:1 (2.5 AU from the Sun), 5:2 (2.8 AU from the Sun), and 2:1 (3.27 AU from the Sun) mean-motion resonances with Jupiter. In a study of V-type asteroids in the middle main belt, however, Roig et al (2008) found that a nonnegligible number of asteroids could be capable of migrating outward across Jupiter's 3:1 resonance, and thus it is conceivable that P/Garradd could be an icy outer-belt asteroid that analogously migrated inward across Jupiter's 5:2 resonance.…”

Section: Mbc Population Sizementioning

confidence: 99%

The Hawaii trails project: comet-hunting in the main asteroid belt

Hsieh

2009

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Context. The mysterious solar system object 133P/(7968) Elst-Pizarro is dynamically asteroidal, yet displays recurrent comet-like dust emission. Two scenarios were hypothesized to explain this unusual behavior: 1) 133P is a classical comet from the outer solar system that has evolved onto a main-belt orbit or 2) 133P is a dynamically ordinary main-belt asteroid on which subsurface ice has recently been exposed. If 1) is correct, the expected rarity of a dynamical transition onto an asteroidal orbit implies that 133P could be alone in the main belt. In contrast, if 2) is correct, other icy main-belt objects should exist and could also exhibit cometary activity. Aims. Believing 133P to be a dynamically ordinary, yet icy main-belt asteroid, I set out to test the primary prediction of the hypothesis: that 133P-like objects should be common and could be found by an appropriately designed observational survey. Methods. I conducted just such a survey -the Hawaii Trails Project -of selected main-belt asteroids in a search for objects displaying cometary activity. Optical observations were made of targets selected from among the Themis, Koronis, and Veritas asteroid families, the Karin asteroid cluster, and low-inclination, kilometer-scale outer-belt asteroids, using the Lulin 1.0 m, small and moderate aperture research telescope system (SMARTS) 1.0 m, University of Hawaii 2.2 m, southern astrophysical research (SOAR) 4.1 m, Gemini North 8.1 m, Subaru 8.2 m, and Keck I 10 m telescopes. Results. I made 657 observations of 599 asteroids, discovering one active object now known as 176P/LINEAR, leading to the identification of the new cometary class of main-belt comets (MBCs). These results suggest that there could be ∼100 currently active MBCs among low-inclination, kilometer-scale outer-belt asteroids. Physically and statistically, MBC activity is consistent with initiation by meter-sized impactors. The estimated rate of impacts and sizes of resulting active sites, however, imply that 133P-sized bodies should become significantly devolatilized over Gyr timescales, suggesting that 133P, and possibly the other MBCs as well, could be secondary, or even multigenerational, fragments from recent breakup events.

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V-type asteroids in the middle main belt

Cited by 68 publications

References 36 publications

SDSS-based taxonomic classification and orbital distribution of main belt asteroids

SDSS-based taxonomic classification and orbital distribution of main belt asteroids

Spectral and mineralogical characterization of inner main-belt V-type asteroids

The Hawaii trails project: comet-hunting in the main asteroid belt

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