DYNAMICAL EVOLUTION OF THE SEINAJOKI ASTEROID FAMILY Vladimir Đošović Bojan Novaković The sixth Symposium "Mathematics and Applications" 17. October2015.

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DYNAMICAL EVOLUTION OF THE SEINAJOKI ASTEROID FAMILY Vladimir Đošović Bojan Novaković The sixth Symposium "Mathematics and Applications" 17. October2015 Faculty of Mathematics, University of Belgrade, Serbia

OUTLINE 1.What are asteroid families? 2.Why are they important? 3.Evolution of asteroid families 4.Aim of this work 5.Secular resonance with Ceres 6.Dynamical models 7.Results 8.Conclusions

WHAT ARE ASTEROID FAMILIES? An asteroid family is a population of asteroids that share similar orbital elements, such as semi-major axis, eccentricity, and inclination. These families are result of a collision among two asteroids. Why fragments stay close to each other after the collision? How can we recognize asteroid families?

WHY ARE THAY IMPORTANT? High energy collisions can not be simulated on Earth Collisional evolution of main asteroid belt Composition of the parent body Families are connected with almost all areas of study of asteroids

DYNAMICAL EVOLUTION OF ASTEROID FAMILIES Evolution of orbital parameters Gravitational effects Non gravitational effects

AIM OF THIS WORK Reconstruction of the complex shape of the Seinajoki asteroid family

(1521) SEINAJOKI FAMILY Family is placed in the outer part of the main asteroid belt Semi-major axis of the family is AU, the orbital inclination of family is a comparatively high, about 15 degrees, with moderate eccentricity of 0.12 The inner edge of the family, in term of semi-major axis, is limited by the strong mean-motion resonance, that is 5:2 with Jupiter Family consists of S type asteroids The Seinajoki asteroid family is also known as Brasilia

SECULAR RESONANCE WITH CERES Motivation for this work comes from recent results about secular resonance with Ceres This resonance is found to cross Seinajoki family

DYNAMICAL MODELS 2 dynamical models are used for integrations These dynamical models are without inner planets Both models include Yarkovsky effect Integrations time span is 200 Myr

INITIAL CONDITIONS Gauss's equation determines the initial ellipse This ellipse denotes the maximum dispersion of fragments immediately after the collision

IMPLEMENTATION OF THE YARKOVSKY EFFECT The Yarkovsky effect is inversely proportional to the diameter of an asteroid Number of test particles corresponds to number of real family members Size of test particles corresponds to size of real family members

RESULTS

CONCLUSIONS Ceres is very important for the evolution The most important parts are explained What is not explained? Two initial families? Role of inner planets?