Collisional Evolution of High-Inclination Asteroids: Implications for Asteroid Strength

Details Collisional Evolution of High-Inclination Asteroids: Implications for Asteroid Strength Collisional Evolution of High-Inclination Asteroids: Implications for Asteroid Strength

Sep 2009

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2009dps....41.2703o&link_type=abstract

American Astronomical Society, DPS meeting #41, #27.03

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Asteroids with inclinations larger than 20 degrees collide with one another, and with lower-inclination asteroids, with a velocity roughly twice as large as the average collisional velocity in the asteroid belt ( 10 km/sec for high-inclination bodies vs. 5 km/sec main belt average). Thus, their size distribution can potentially evolve differently than the main belt as a whole, for two reasons: 1) the larger collision velocity means that a smaller impactor can lead to their catastrophic disruption; and 2) the energy needed for catastrophic disruption is likely a function of collision velocity [1].
Using a collisional evolution model [2,3] modified to treat two interacting populations, as well as new velocity-dependent scaling laws for asteroid collisional disruption, we study the possible differences in the size distribution of high-inclination asteroids that may result from their increased collision velocity. Recent observations suggest that the size distribution of asteroids around a kilometer in diameter may be shallower for high-inclination asteroids than for low-inclination asteroids [4]. We will discuss the implications that such observational constraints have for the collisional properties of asteroids, namely their strength against catastrophic disruption and how it varies with impact velocity.
References: [1] Benz and Asphaug (1999), Icarus 142, 5-20. [2] Bottke et al. (2005), Icarus 175, 111-140. [3] O'Brien (2009), Icarus, in press. [4] Terai and Itoh (2008), ACM 2008, abstract #8215.

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