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The other Eunomian asteroids are quite regularly distributed in orbital space around Eunomia. The next largest member identified by the analysis was 258 Tyche of 65 km diameter. However, its orbit lies at the very margin of what can be considered the family region, and it may well be an interloper. The largest clear family members are about 30 km diameter, with several asteroids in this size range.
Spectroscopic studies have shown that the family members span a noticeable range of compositions, although all remain within the S-type asteroid. As such they are of generally stony (rather than icy) surface composition that includes and some nickel-iron, and are quite bright for their size.
The family contains relatively large numbers of small objects. Since most of these smaller objects are "eroded" away over time due to secondary collisions, gravitational perturbations, and the Yarkovsky effect, this indicates that the Eunomia family was created relatively recently (on an astronomical timescale).
The Cassini-Huygens spacecraft flew by 2685 Masursky, a small family member, in 2000. However, the encounter distance of about one million kilometers was too large for surface features to be resolved.
A HCM numerical analysis by Zappalà, et al. determined a large group of 'core' family members, whose proper orbital elements lie in the approximate ranges
| p'' !! ''[[ip>inclination]]'' |
| 11.6° |
| 14.8° |
| 11.1° |
| 15.8° |
The Zappalà 1995 analysis found 439 core members, while a search of a recent proper element database for 96944 in 2005 yielded 4649 objects lying within the rectangular-shaped region defined by the first table above. By 2014, Nesvorný identified at total of 5,670, or approximately 1.4% of all asteroids, using the Hierarchical Clustering Method.
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