MIDI observations of 1459 Magnya: First attempt of interferometric observations of asteroids with the VLTI

Delbò, M.; Gai, M.; Ligori, S.; Loreggia, D.; Saba, L.; Cellino, A.; Licchelli, D.; Blanco, C.; Cigna, M.; Wittkowski, M.

doi:10.1016/j.icarus.2006.01.001

Cited by 27 publications

(16 citation statements)

References 19 publications

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“…3). The calculated sizes of Vesta family members assume an albedo of 0.4, consistent with that of Vesta (Tedesco et al 2002) and Magnya, another basaltic asteroid (Delbo et al 2006). The size distribution of the Vesta family below about 3 km diameter (dotted line) is likely incomplete and may not be representative of the true size distribution in that range the family, placing a minimum age of 1 Gyr on the Vesta family.…”

Section: Vesta's Familysupporting

confidence: 54%

The Origin and Evolution of the Asteroid Belt—Implications for Vesta and Ceres

O’Brien

Sykes

2011

Space Sci Rev

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Vesta and Ceres are the largest members of the asteroid belt, surviving from the earliest phases of Solar System history. They formed at a time when the asteroid belt was much more massive than it is today and were witness to its dramatic evolution, where planetary embryos were formed and lost, where the collisional environment shifted from accretional to destructive, and where the current size distribution of asteroids was sculpted by mutual collisions and most of the asteroids originally present were lost by dynamical processes. Since these early times, the environment of the asteroid belt has become relatively quiescent, though over the long history of the Solar System the surfaces of Vesta and Ceres continue to record and be influenced by impacts, most notably the south polar cratering event on Vesta. As a consequence of such impacts, Vesta has contributed a significant family of asteroids to the main belt, which is the likely source of the HED meteorites on Earth. No similar contribution to the main belt (or meteorites) is evident for Ceres. Through studies of craters, the surfaces of these asteroids will offer an opportunity for Dawn to probe the modern population of small asteroids in a size regime not directly observable from Earth.

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Section: Vesta's Familysupporting

confidence: 54%

The Origin and Evolution of the Asteroid Belt—Implications for Vesta and Ceres

O’Brien

Sykes

2011

Space Sci Rev

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“…The albedo may be as high as 0.42, like that of (4) Vesta, or as low as 0.21, like that of (1459) Magnya according to Tedesco et al (2002). It is noteworthy, however, that more recent determinations give a value of 0.37 for (1459) Magnya (Delbó et al 2006), which is the only other V-type asteroid with a known geometric albedo. A radius of about 4 km would also be obtained using the albedo of (15) Eunomia.…”

Section: Yarkovsky Evolutionmentioning

confidence: 93%

On the V-type asteroids outside the Vesta family

Carruba¹,

Michtchenko²,

Lazzaro³

2007

A&A

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Context. The V-type asteroids are associated with basaltic composition. Apart from (1459) Magnya, an asteroid that is clearly dynamically and mineralogically unconnected to the Vesta family, all currently known V-type asteroids are either members of the Vesta family, or are hypothesized to be former members of the dynamical family that migrated to their current orbital positions. The recent identification of (21238) 1995 WV7 as a V-type asteroid introduces the possibility that a second basaltic asteroid not connected with the Vesta family exists. This asteroid is on the opposite side of the 3:1 mean motion resonance with respect to Vesta, and it would be very unlikely that a member of the Vesta family of its size (D > 5 km) migrating via either the Yarkovsky effect or repeated close encounters with Vesta survived the passage through such a resonance. Aims. In this work we investigate the possibility that (21238) 1995 WV7 originated as a fragment of the parent body of the Eunomia family and then migrated via the interplay of the Yarkovsky effect and some powerful nonlinear secular resonances, such as the (s − s 6 ) − (g 5 − g 6 ). If (15) Eunomia is, as claimed, a differentiated object whose originally pyroxene-enriched crust layer was lost in a collision that either created the Eunomia family or preceded its formation, can (21238) be a fragment of its long-lost basaltic crust that migrated to the current position? Methods. We mapped the phase space around (21238) and determined which of the nonlinear secular resonances that we identified are stronger and more capable of having caused the current difference in proper i between (21238) and members of the Eunomia family. We simulated the Yarkovsky effect by using the SWIFT-RMVSY integrator. Results. Our results suggest that it is possible to migrate from the Eunomia dynamical family to the current orbital location of (21238) via the interplay of the Yarkovsky effect and the (s − s 6 ) − (g 5 − g 6 ) nonlinear secular resonance, on time-scales of at least 2.6 Gyr. Conclusions. (15) Eunomia might be the third currently known parent body for V-type asteroids.

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“…Ages are derived according to the collisional evolution of main belt asteroids (Bottke et al 2005;Marchi et al 2006b). Collisional lifetimes depend upon the diameters, which have been estimated using the measured average geometric albedo (0.3) of a sample of V-types (Tedesco et al 2002;Benner et al 2002;Delbó et al 2003Delbó et al , 2006. The collisional age of V-types spans from about 0.5 to 2.7 Ga.…”

Section: Parameterizing the Space Weatheringmentioning

confidence: 99%

On the Puzzle of Space Weathering Alteration of Basaltic Asteroids

Marchi

Sanctis²,

Lazzarin

et al. 2010

ApJ

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The majority of basaltic asteroids are found in the inner main belt, although a few have also been observed in the outer main belt and near-Earth space. These asteroids-referred to as V-types-have surface compositions that resemble that of the 530 km sized asteroid Vesta. Besides the compositional similarity, dynamical evidence also links many V-type asteroids to Vesta. Moreover, Vesta is one of the few asteroids to have been identified as source of specific classes of meteorites, the howardite, eucrite, and diogenite achondrites (HEDs). Despite the general consensus on the outlined scenario, several questions remain unresolved. In particular, it is not clear if the observed spectral diversity among Vesta, V-types, and HEDs is due to space weathering, as is thought to be the case for S-type asteroids. In this Letter, SDSS photometry is used to address the question of whether the spectral diversity among candidate V-types and HEDs can be explained by space weathering. We show that visible spectral slopes of V-types are systematically redder with respect to HEDs, in a similar way to what is found for ordinary chondrite meteorites and S-types. On the assumption that space weathering is responsible for the slope mismatch, we estimated an upper limit for the reddening timescale of about 0.5 Ga. Nevertheless, the observed slope mismatch between HEDs and V-types poses several puzzles to understanding its origin. The implication of our findings is also discussed in light of the Dawn mission to Vesta.

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MIDI observations of 1459 Magnya: First attempt of interferometric observations of asteroids with the VLTI

Cited by 27 publications

References 19 publications

The Origin and Evolution of the Asteroid Belt—Implications for Vesta and Ceres

The Origin and Evolution of the Asteroid Belt—Implications for Vesta and Ceres

On the V-type asteroids outside the Vesta family

On the Puzzle of Space Weathering Alteration of Basaltic Asteroids

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