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Fig. 4


Dependence of the pole latitude β on the proper semi-major axis ap for eight studied asteroid families: Flora, Koronis, Eos, Eunomia, Phocaea, Themis, Maria, and Alauda. Family members are marked by circles and borderline cases by squares, whose sizes are scaled proportionally to diameters. Only the scale for (15) Eunomia was decreased by half to fit the figure. The vertical lines correspond to the likely centers of the asteroid families, whose uncertainties are usually < 0.01 AU. The Eos family has an asymmetric V-shape (the (ap, H) border is asymmetric), which makes the center determination harder, so we marked two possible positions. One corresponds to the right (ap, H) border, the second to the left border. The uncertainties in β are usually 5–20°. In most cases, the value of |β| ≳ 30°, hence the quadrant to which the asteroid belongs (defined by the center of the family and the value β = 0°), is not changed.

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