In physics, specifically general relativity, the Mathisson–Papapetrou–Dixon equations describe the motion of a massive spinning body moving in a gravitational field. Other equations with similar names and mathematical forms are the Mathisson–Papapetrou equations and Papapetrou–Dixon equations. All three sets of equations describe the same physics. These equations are named after Myron Mathisson, William Graham Dixon, and Achilles Papapetrou, who worked on them. Throughout, this article uses the natural units c = G = 1, and tensor index notation.
Mathisson–Papapetrou–Dixon equations The Mathisson–Papapetrou–Dixon (MPD) equations for a mass m {\displaystyle m} spinning body are
D k ν D τ + 1 2 S λ μ R λ μ ν ρ V ρ = 0 , D S λ μ D τ + V λ k μ − V μ k λ = 0. {\displaystyle {\begin{aligned}{\frac {Dk_{\nu }}{D\tau }}+{\frac {1}{2}}S^{\lambda \mu }R_{\lambda \mu \nu \rho }V^{\rho }&=0,\\{\frac {DS^{\lambda \mu }}{D\tau }}+V^{\lambda }k^{\mu }-V^{\mu }k^{\lambda }&=0.\end{aligned}}}
Here τ {\displaystyle \tau } is the proper time along the trajectory, k ν {\displaystyle k_{\nu }} is the body's four-momentum
k ν = ∫ t = const T 0 ν g d 3 x , {\displaystyle k_{\nu }=\int _{t={\text{const}}}{T^{0}}_{\nu }{\sqrt {g}}d^{3}x,}
the vector V μ {\displaystyle V^{\mu }} is the four-velocity of some reference point X μ {\displaystyle X^{\mu }} in the body, and the skew-symmetric tensor S μ ν {\displaystyle S^{\mu \nu }} is the angular momentum
S μ ν = ∫ t = const { ( x μ − X μ ) T 0 ν − ( x ν − X ν ) T 0 μ } g d 3 x {\displaystyle S^{\mu \nu }=\int _{t={\text{const}}}\left\{\left(x^{\mu }-X^{\mu }\right)T^{0\nu }-\left(x^{\nu }-X^{\nu }\right)T^{0\mu }\right\}{\sqrt {g}}d^{3}x}
… excerpt ends here. Continue reading the full article.

