TheMassalia family (adj.Massalian;FIN:404) is afamily ofasteroids in the innerasteroid belt, named after itsparent body,20 Massalia. It consists ofS-type asteroids with very lowinclinations, straddling the 1:2resonances withMars. There are more than 6,000 known Massalian asteroids.[1]
This is a definite cratering family consisting of20 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 100 to 200 million years ago. It has a distinctly two-lobed appearance in propera--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 theYarkovsky andYORP effects. Details of the lobes were used to calculate the age of the family.[2]
A strong 1:2orbital resonance withMars crosses the family at 2.42AU, and appears responsible for some "leakage" of family members away from the area into higher inclination orbits.[2]
The Massalia family or a recent minor collision within it may be the source for the prominent αdust band, the other candidate being a recent collision within theThemis family.[2][3]
The Massalian asteroids are located at very low inclinations, straddling the 1:2resonances withMars.
AHCM numerical analysis by Zappalà in 1995,[4] determined a group of core family members, whoseproper orbital elements lie in the approximate ranges
| ap | ep | ip | |
|---|---|---|---|
| min | 2.37AU | 0.143 | 1.2° |
| max | 2.45 AU | 0.175* | 1.75° |
At the presentepoch, the range ofosculatingorbital elements of these core members is
| a | e | i | |
|---|---|---|---|
| min | 2.37AU | 0.124 | 0.4° |
| max | 2.45 AU | 0.211 | 2.35° |
The analysis by Zappalà found 42 core members in 1995,[4] while a HCM-analysis by Nesvorný in 2014 yielded 6,424 member asteroids based on the proper elements of acatalog of 398,000 bodies.[1]: 23
| Name/designation | Number | Proper semimajor axis (AU) | Proper inclination (degrees) | Proper eccentricity | Diameter (km) | Group |
|---|---|---|---|---|---|---|
| Massalia | 20 | 2.409 | 1.421 | 0.162 | 150 (measured) | Primary member |
| Muchachos | 2946 | 2.455 | 1.417 | 0.166 | 9 (estimated) | Interloper |
| Puccini | 4579 | 2.400 | 1.392 | 0.163 | 8 (estimated) | Core member |
| Rameau | 4734 | 2.416 | 1.359 | 0.164 | 5 (estimated) | Core member |
| Švejcar | 5031 | 2.436 | 1.535 | 0.148 | 7 (estimated) | Interloper |
| Hessen | 5846 | 2.435 | 0.913 | 0.163 | 5 (estimated) | Interloper |
| 1990 RW3 | 7760 | 2.407 | 1.465 | 0.156 | 9 (estimated) | Core member |
A number ofInterlopers have been identified, which share the same orbital elements as the true family members, but cannot have come from the same cratering event because of spectral (hence, compositional) differences.2946 Muchachos and some other bodies were noted as interlopers during a detailed study of the family,[2] while2316 Jo-Ann is seen to have the wrong spectrum by inspection of thePDS asteroid taxonomy data set. Muchachos is larger than any of the true family members apart from Massalia itself.