An Introduction to the Equatorial Orbitals of Toy Neutron Stars Aubrey Truman ∗ Department of Mathematics, Computational Foundry, Swansea University Bay Campus, Fabian Way, Swansea, SA1 8EN, UK September 16, 2019 Abstract In modelling the behaviour of ring systems for neutron stars in a non-relativistic setting one has to combine Newton’s inverse square law of force of gravity with the Lorentz force due to the magnetic dipole moment in what we refer to as the KLMN equation. Here we investigate this problem using analytical dynamics revealing a strong link between Weierstrass functions and equatorial orbitals. The asymptotics of our solutions reveal some new physics involving unstable circular orbits with possible long term effects - doubly asymp- totic spirals, the hyperbolic equivalent of Keplerian ellipses in this set- ting. The corresponding orbitals can only arise when the discriminant of a certain quartic, Q; ∆4 = 0. When this occurs simultaneously with g3, its quartic invariant, changing sign, the physics changes dramat- ically. Here we introduce dimensionless variables Z and W for this problem, ∆4(Z; W ) = 0, is then an algebraic plane curve of degree 6 whose singularities reveal such changes in the physics. The use of polar coordinates displays this singularity structure very clearly. Our first result shows that a time-change in the equations ofmo- tion leads to a complete solution of this problem in terms of Weier- strass functions. Since Weierstrass’s results underlie this entire work we present this result first. Legendre’s work leads to a complete solu- tion. Both results reinforce the physical importance of the condition, ∗Email:
[email protected] 1 ∆4 = 0, our final flourish being provided by Jacobi with his theta function.