SolarGravityAndRadiationPressure¶
- class sbpy.dynamics.models.SolarGravityAndRadiationPressure(**kwargs)[source] [edit on github]¶
Bases:
DynamicalModelEquation of motion solver for a particle orbiting the Sun, including radiation force.
Dust is parameterized with
beta, the ratio of the force from solar radiation pressure (\(F_r\)) to that from solar gravity (\(F_g\)):\[\beta = \frac{{F_r}}{{F_g}}\]For spherical dust grains,
betareduces to:\[\beta = \frac{{0.57 Q_{{pr}}}}{{\rho a}}\]where \(Q_{{pr}}\) is the radiation pressure efficiency averaged over the solar spectrum, \(\rho\) is the mass density of the grain (g/cm3), and \(a\) is the grain radius (μm) (Burns et al. 1979).
Only Newtonian gravity and radiation pressure are considered. Poynting-Roberston drag and general relativity are not included.
- Parameters:
- **kwargs
dict Arguments passed on to
solve_ivp. Units are seconds, km, and km/s, e.g.,max_stepis a float value in units of seconds. For relative and absolute tolerance keywords,rtolandatol, 6-element arrays may be used, where the first three elements are for position, and the last three are for velocity.
- **kwargs
Attributes Summary
Gravitational constant times mass.
Methods Summary
df_drv(t, rv, beta, *args)dx_dt(t, rv, beta, *args)solve(initial, t_final, *args)Solve the equations of motion for a single particle.
Attributes Documentation
- GM¶
Gravitational constant times mass.
Methods Documentation
- solve(initial: State, t_final: Time, *args) State [edit on github]¶
Solve the equations of motion for a single particle.
The solution is calculated with
scipy.integrate.solve_ivp.- Parameters:
- Returns:
- final
State
- final