Computational perturbative methods for Hamiltonian systems – Applications in physics and astronomy. A Conference in Athens, Greece, 11-13 July 2016
The decision to organize this meeting was taken after noting that there has been since long a number of groups developing diverse symbolic tools or computer-algebraic methods for implementing Hamiltonian perturbation theory in various contexts of mathematical or physical interest. These methods have already reached a state of maturity, and their implementation has yielded a number of results of particular importance both in the theory and in the applications of Hamiltonian systems. Our aim is to assemble together colleagues, in order to discuss these developments, their own work, as well as future prospects in this promising field of research.
Simulation of the interaction of a disc with a satellite galaxy via the newly developed MAIN code (Mesh-adaptive Approximate Inverse N-body code).
The disc galaxy has a mass of 5 X 10^10 solar masses, and it is embedded in a live dark halo of 10^11 solar masses. The satellite galaxy has a mass of 10^10 solar masses. The disc' spiral structure is generated by a companion's pericentric passage at about 15Kpc from the disc's center. The spiral structure is maintained for about six revolutions. At later stages, the companion falls into the disc due to dynamical friction with the halo.
The MAIN code was developed as a collaboration between the RCAAM (C. Efthymiopoulos, P. Patsis) and the scientific computation group of the Department of Electrical and Computer Engineering of the Democritus University of Thrace (P. Kyziropoulos, G. Gravvanis).