(15) Eunomia as a Possible Past Source for Middle Main Belt V-type Asteroids

Details (15) Eunomia as a Possible Past Source for Middle Main Belt V-type Asteroids (15) Eunomia as a Possible Past Source for Middle Main Belt V-type Asteroids

Oct 2007

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2007dps....39.5103l&link_type=abstract

American Astronomical Society, DPS meeting #39, #51.03; Bulletin of the American Astronomical Society, Vol. 39, p.515

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Scientific paper

The V-type asteroids are associated with basaltic composition. Apart from (1459) Magnya, 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 positions. The recent identification of (21238) 1995 WV7, (40521) 1999 RL95, and (possibly) of (66905) 1999 VC160 as V-type asteroids in the middle main belt introduces the possibility of another basaltic asteroid not connected with the Vesta family. These asteroids are 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 (21238) size (D>5 km) survived the passage through the resonance.
In this work we investigate the possibility that all three asterids originated as membera of the Eunomia family and then migrated via the interplay of the Yarkovsky effect and some powerful nonlinear secular resonances. 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, then the new discovered V-type asteroids could be fragments of the long-lost basaltic crust of the Eunomia family parent body.
We mapped the phase space around all three asteroids and determined which of the identified nonlinear secular resonances are stronger and more capable of having caused the current difference in proper i between these and members of the Eunomia family.
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-s6)-(g5-g6) nonlinear secular resonance, on time-scales of at least 2.6 Gyr. (15) Eunomia might be the third currently known parent body for V-type asteroids.

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