Zodiacal dust bands: Their relation to asteroid families

摘要: Abstract A mathematical model of the spatial distribution orbitally evolved collisional debris which reproduces zodiacal dust band phenomenon is developed. The resultant torus has maxima in particle density at heliocentric latitudes near mean proper orbital inclinations its constituent particles, and loci perihelia aphelia orbits. These perihelion aphelion pairs are found to have latitudinal radial separations functions elements ( a , e i ) constitutent as well dispersions those elements. Models tori associated with seven asteroid families generated compared observations principal bands. It that models Themis Koronis consistent innermost observed bands, α β, respectively. γ particles (seen ∼8.°3 ecliptic latitude) best fit by an Eos family having dispersion inclination ∼1.°4, value ∼0.°7 for asteroids. Dispersions smal (10–100 μm) expected be larger than population due greater frequency relevant collisions among former. Other detected bands not association other major possible exception Io family. This suggests solely local peaks volume known asteroids, would from mechanism uniformly eroding whole, but rather supports theory they were produced consequence large random individual asteroids (the largest also resulted observable families). Such nonequilibrium further supported evidence Nonequilibrium production evolution offer framework within all can understood. Within this framework, it both much older Dust appear experienced any decay (less few tenths AU) Poynting-Robertson drag.