Radiation-driven Life-cycle of Small Binaries

Details Radiation-driven Life-cycle of Small Binaries Radiation-driven Life-cycle of Small Binaries

Oct 2007

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2007dps....39.0508c&link_type=abstract

American Astronomical Society, DPS meeting #39, #5.08; Bulletin of the American Astronomical Society, Vol. 39, p.417

Astronomy and Astrophysics

Astronomy

Scientific paper

Recent discovery of abundant small MBA binaries (Pravec and Harris 2006) and a more self-consistent reassessment of effects of planetary encounters (Walsh and Richardson 2007) suggest that planetary encounters are likely not the main mechanism for formation of near-Earth asteroid (NEA) binaries. Binary formation through the YORP effect (Bottke et al. 2002) is now the leading candidate for a common NEA and main-belt binary formation mechanims. In Cuk (2007) I show that the mass loss from the primary's surface due to YORP is sufficient to acount for the formation of kilometer-sized binary NEAs. I also propose that the small-separation NEA binaries' observed properties are consistent with evolution through "binary YORP," rather than tidal stripping during planetary passages. Such a life cycle implies that most small binary asteroids must be extremely young, with ages <10^5 yr.

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