Orbital motion in space from the conservation laws: the shape of the orbit falls out of the Eccentricity Vector without integrating anything.

Orbital Motion From Conservation Laws

  1. Rearrange the eccentricity vector:
    • 𝐞+̂𝐫=̇𝐫×𝐡𝜇
  2. Dot with 𝐫 and use the scalar triple product:
    • 𝐫⋅𝐞+𝑟=1𝜇𝐫⋅(̇𝐫×𝐡)=1𝜇(𝐫×̇𝐫)⏟𝐡⋅𝐡=ℎ2𝜇
  3. With 𝜃 the angle from 𝐞 to 𝐫, 𝐫⋅𝐞=𝑟𝑒cos𝜃:
    • 𝑟(1+𝑒cos𝜃)=ℎ2𝜇=𝑝
    • 𝑝 is the semi-latus rectum
    • 𝑒=|𝐞| is the eccentricity

Terminology

  • “anomaly”, “argument” = angle
  • 𝜃 is the true anomaly: the angle from the eccentricity vector (perigee) to the satellite

The Orbit Equation

Orbit Equation

  • 𝑟=𝑝1+𝑒cos𝜃
  • Curtis (2.45)
  • Relates 𝑟, the geocentric distance, to 𝜃, the true anomaly
  • Closest approach (perigee) at 𝜃=0, farthest (apogee) at 𝜃=𝜋 when 𝑒<1
  • Writing it in Cartesian coordinates shows the orbit is a conic section (Kepler’s first law)