Massalia family

The Massalia or Massalian family of asteroids is a grouping of S-type asteroids in the inner main belt at very low inclination. About 0.8% of known asteroids belong to this family.

This is a definite cratering family consisting of 20 Massalia and a mass of small fragments excavated from Massalia's surface by an impact. Massalia is by far the largest member with a diameter of about 150 km, while the next largest body, (7760) 1990 RW3 is only about 7 km in diameter. The mass of all the small members is negligible, less than about 1%, compared to Massalia.

The family is fairly young, estimated to have been created by an impact 150 to 200 million years ago. It has a distinctly two-lobed appearance in proper a--e space, with one lobe centered at semi-major axes of 2.38 AU, the other at about 2.43 AU, with the parent body Massalia itself located in between. The bodies in the lobes tend to be smaller on average than those in the central region. It has been shown that this structure is likely caused by slow drift of the semi-major axis caused by the Yarkovsky and YORP effects. Details of the lobes were used to calculate the age of the family.

A strong 1:2 orbital resonance with Mars crosses the family at 2.42 AU, and appears responsible for some "leakage" of family members away from the area into higher inclination orbits.

The Massalia family or a recent minor collision within it may be the source for the prominent α dust band, the other candidate being a recent collision within the Themis family.

The Massalian asteroids are located at very low inclinations, straddling the 1:2 resonances with Mars.

A HCM numerical analysis by Zappalà et al. determined a group of 'core' family members, whose proper orbital elements lie in the approximate ranges

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