The shallow magnitude distribution of asteroid families

Details The shallow magnitude distribution of asteroid families The shallow magnitude distribution of asteroid families

Apr 2003

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2003icar..162..328m&link_type=abstract

Icarus, Volume 162, Issue 2, p. 328-336.

Computer Science

21

Scientific paper

It is well known that asteroid families have steeper absolute magnitude (H) distributions for H < 12-13 values than the background population. Beyond this threshold, the shapes of the absolute magnitude distributions in the family/background populations are difficult to determine, primarily because both populations are not yet observationally complete. Using a recently generated catalog containing the proper elements of 106,284 main belt asteroids and an innovative approach, we debiased the absolute magnitude distribution of the major asteroid families relative to the local background populations. Our results indicate that the magnitude distributions of asteroid families are generally not steeper than those of the local background populations for H > 13 (i.e., roughly for diameters smaller than 10 km). In particular, most families have shallower magnitude distributions than the background in the range 15-17 mag. Thus, we conclude that, contrary to previous speculations, the population of kilometer-size asteroids in the main belt is dominated by background bodies rather than by members of the most prominent asteroid families. We believe this result explains why the Spacewatch, Sloan Digital Sky Survey, and Subaru asteroid surveys all derived a shallow magnitude distribution for the dimmer members of the main belt population.
We speculate on a few dynamical and collisional scenarios that can explain this shallow distribution. One possibility is that the original magnitude distributions of the families (i.e., at the moment of the formation event) were very shallow for H larger than ~ 13, and that most families have not yet had the time to collisionally evolve to the equilibrium magnitude distribution that presumably characterizes the background population. A second possibility is that family members smaller than about 10 km, eroded over time by collisional and dynamical processes, have not yet been repopulated by the break-up of larger family members. For this same reason, the older (and possibly characterized by a weaker impact strength) background population shows a shallow distribution in the range 15-60 km.

Affiliated with

Also associated with

No associations

Rating

The shallow magnitude distribution of asteroid families does not yet have a rating. At this time, there are no reviews or comments for this scientific paper.

If you have personal experience with The shallow magnitude distribution of asteroid families, we encourage you to share that experience with our LandOfFree.com community. Your opinion is very important and The shallow magnitude distribution of asteroid families will most certainly appreciate the feedback.

Rate now

Comments { 0 }

Profile ID: LFWR-SCP-O-848747