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Title:
Signatures of Recent Asteroid Disruptions in the Formation and Evolution of Solar System Dust Bands
Authors:
Espy Kehoe, A. J.; Kehoe, T. J. J.; Colwell, J. E.; Dermott, S. F.
Affiliation:
AA(Department of Physics, University of Central Florida, 4000 Central Florida Blvd, Building 121, PS 430, Orlando, FL 32816-2385, USA 0000-0003-2870-2066), AB(Departamento de Física da Universidade de Aveiro and CIDMA Campus de Santiago, 3810-183 Aveiro, Portugal; Florida Space Institute, 12354 Research Parkway, Partnership 1 Building, Suite 214, Orlando, FL 32826-2933, USA), AC(Department of Physics, University of Central Florida, 4000 Central Florida Blvd, Building 121, PS 430, Orlando, FL 32816-2385, USA), AD(Department of Astronomy, University of Florida, 211 Bryant Space Science Center, Gainesville, FL 32611-2055, USA)
Publication:
The Astrophysical Journal, Volume 811, Issue 1, article id. 66, 16 pp. (2015). (ApJ Homepage)
Publication Date:
09/2015
Origin:
IOP
Astronomy Keywords:
celestial mechanics, minor planets, asteroids: general, planets and satellites: dynamical evolution and stability, zodiacal dust
DOI:
10.1088/0004-637X/811/1/66
Bibliographic Code:
2015ApJ...811...66E

Abstract

We have performed detailed dynamical modeling of the structure of a faint dust band observed in coadded InfraRed Astronomical Satellite data at an ecliptic latitude of 17° that convincingly demonstrates that it is the result of a relatively recent (significantly less than 1 Ma) disruption of an asteroid and is still in the process of forming. We show here that young dust bands retain information on the size distribution and cross-sectional area of dust released in the original asteroid disruption, before it is lost to orbital and collisional decay. We find that the Emilkowalski cluster is the source of this partial band and that the dust released in the disruption would correspond to a regolith layer ˜3 m deep on the ˜10 km diameter source body's surface. The dust in this band is described by a cumulative size-distribution inverse power-law index with a lower bound of 2.1 (implying domination of cross-sectional area by small particles) for dust particles with diameters ranging from a few mum up to a few cm. The coadded observations show that the thermal emission of the dust band structure is dominated by large (mm-cm size) particles. We find that dust particle ejection velocities need to be a few times the escape velocity of the Emilkowalski cluster source body to provide a good fit to the inclination dispersion of the observations. We discuss the implications that such a significant release of material during a disruption has for the temporal evolution of the structure, composition, and magnitude of the zodiacal cloud.
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