A Frequency Approach To Identifying Asteroid Families: Families Interacting With Nonlinear Secular Resonances And Low-order Mean-motion Resonances

Details A Frequency Approach To Identifying Asteroid Families: Families Interacting With Nonlinear Secular Resonances And Low-order Mean-motion Resonances A Frequency Approach To Identifying Asteroid Families: Families Interacting With Nonlinear Secular Resonances And Low-order Mean-motion Resonances

Sep 2008

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2008dps....40.5204c&link_type=abstract

American Astronomical Society, DPS meeting #40, #52.04; Bulletin of the American Astronomical Society, Vol. 40, p.492

Astronomy and Astrophysics

Astronomy

Scientific paper

In Carruba and Michtchenko (2007) we introduced a method for asteroid family determination where families were identified in the proper frequency domain (n,g,g+s)(where n is the mean-motion, and g and s are the secular frequencies of the longitudes of pericenter and nodes, respectively), rather than in the proper element domain (a,e,i) (semi-major axis, eccentricity and inclination). The reason for the choice of the (n,g,g+s) domain was that i) the g+s frequency combination as a function of the mean-motion n is almost constant (Milani and Knezevic, 1994) and ii) this metric was ideal for studying families interacting with secular resonances of argument g+s, such as the g-g6+s-s6. However, i) not all families are crossed by a g+s secular resonance, and ii) low-order mean-motion resonances have a perturbing effect on the g frequency. In particular, g may not follow a linear trend as a function of n near mean-motion resonance borders, or may be negative (or retrograde) for asteroids locked in resonant configurations such as the Hildas in the 3J:2A resonance.
Here we improve our techniques for identifying members of families in mean-motion resonant configurations. We introduce several new distance metrics in frequency spaces optimal for identifying objects that diffused in secular resonances of argument 2g-s, 3g-s, g-s, s, and 2s. We also regularize the dependence of the g frequency as a function of the n frequency (Vesta family) or of the eccentricity e (Hansa family).
Our approaches allow to recognize as family members objects that were lost with previous methods, while keeping the advantages of the Carruba and Michtchenko (2007) approach. More important, an analysis in the frequency domain furnish a deeper understanding of the dynamical evolution of asteroid families not always obtainable with an analysis in the proper element domain.

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