We extend the canonical formalism for the motion of N particles in lineal gravity to include charges. Under suitable coordinate conditions and boundary conditions the Hamiltonian is defined as the spatial integral of the second derivative of the dilaton field which is given as a solution to the constraint equations. For a system of two particles the determining equation of the Hamiltonian (a kind of transcendental equation) is derived from the matching conditions for the dilaton field at the particles' position. The canonical equations of motion are derived from this determining equation. For the equal mass case the canonical equations in terms of the proper time can be exactly solved in terms of hyperbolic and/or trigonometric functions. In electrodynamics with zero cosmological constant the trajectories for repulsive charges exhibit not only bounded motion but also a countably infinite series of unbounded motions for a fixed value of the total energy H0, while for attractive charges the trajectories are simply periodic. When the cosmological constant Λ is introduced, the motion for a given Λ and H0 is classified in terms of the charge-momentum diagram from which we can predict what type of the motion is realized for a given charge. In general the cosmological constant acts on the particles as a repulsive (Λ>0) or an attractive (Λ<0) potential. But for a certain range of Λ<0, small q and small mass the trajectory shows a double peak structure due to an interplay among the induced momentum dependent Λ potential, the gravitational attraction and the relativistic effect. For Λ>0, depending on the value of charge, only bounded motion or the infinite series of unbounded motion or both are realized. Since in this theory the charge of each particle appears in the form e1e2 in the determining equation, the static balance condition in 1+1 dimensions turns out to be identical with the condition in Newtonian theory. We generalize this condition to nonzero momenta, obtaining the first exact solution to the static balance problem that does not obey the Majumdar–Papapetrou condition.
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