implementations.problem_classes.OuterSolarSystem module¶
- class outer_solar_system(sun_only=False)[source]¶
Bases:
ptypeThe \(N\)-body problem describes the mutual influence of the motion of \(N\) bodies. Formulation of the problem is based on Newton’s second law. Therefore, the \(N\)-body problem is formulated as
\[m_i \frac{d^2 {\bf r}_i}{d t^2} = \sum_{j=1, i\neq j}^N G \frac{m_i m_j}{|{\bf r}_i - {\bf r}_j|^3}({\bf r}_i - {\bf r}_j),\]where \(m_i\) is the \(i\)-th mass point with position described by the vector \({\bf r}_i\), and \(G\) is the gravitational constant. If only the sun influences the motion of the bodies gravitationally, the equations become
\[m_i \frac{d^2 {\bf r}_i}{d t^2} = G \frac{m_1}{|{\bf r}_i - {\bf r}_1|^3}({\bf r}_i - {\bf r}_1).\]This class implements the outer solar system consisting of the six outer planets: the sun, Jupiter, Saturn, Uranus, Neptune, and Pluto, i.e., \(N=6\).
- Parameters:
sun_only (bool, optional) – If False, only the sun is taken into account for the influence of the motion.
- G¶
Gravitational constant.
- Type:
float
- G = 0.000295912208286¶
- dtype_f¶
alias of
acceleration
- dtype_u¶
alias of
particles
- eval_f(u, t)[source]¶
Routine to compute the right-hand side of the problem.
- Parameters:
u (dtype_u) – The particles.
(float) (t)
- Returns:
me – The right-hand side of the problem.
- Return type:
dtype_f