The most common is to scale by mk to define the eccentricity vector e = A m k = 1 m k ( p × L ) − r ^   . {\displaystyle \mathbf {e} ={\frac {\mathbf {A} }{mk}}={\frac {1}{mk}}(\mathbf {p} \times \mathbf {L} )-\mathbf {\hat {r}} ~.} The shape and orientation of the Kepler problem orbits can be determined from the LRL vector as follows.
Cea mai comună este de a scala prin mk pentru a defini vectorul excentricitate e = A m k = 1 m k ( p × L ) − r ^   . {\displaystyle \mathbf {e} ={\frac {\mathbf {A} }{mk}}={\frac {1}{mk}}(\mathbf {p} \times \mathbf {L} )-\mathbf {\hat {r}} ~.} Forma si orientarea orbitelor din problemele de tip Kepler pot fi determinate pornind de la vectorul LRL,A , după cum urmează.