# Specific relative angular momentum

*See also: Classical central-force problem*

In celestial mechanics, the **specific relative angular momentum (h)** of two orbiting bodies is the vector product of the relative position and the relative velocity. Equivalently, it is the total angular momentum divided by the reduced mass.^{[1]} Specific relative angular momentum plays a pivotal role in the analysis of the two-body problem.

## Definition

Specific relative angular momentum, represented by the symbol , is defined as the cross product of the relative position vector and the relative velocity vector .

where:

- is the relative orbital position vector
- is the relative orbital velocity vector
- is the total angular momentum of the system (i.e. the sum of the angular momenta of each body)
- is the reduced mass

The units of are **m ^{2}s^{−1}**.

The vector is always perpendicular to the instantaneous osculating orbital plane, which coincides with the instantaneous perturbed orbit. It would not necessarily be perpendicular to an average plane which accounted for many years of perturbations.

As usual in physics, the magnitude of the vector quantity is denoted by :

## Elliptical orbit

In an elliptical orbit, the specific relative angular momentum is twice the area per unit time swept out by a chord from the primary to the secondary: this area is referred to by Kepler's second law of planetary motion.

Since the area of the entire orbital ellipse is swept out in one orbital period, is equal to twice the area of the ellipse divided by the orbital period, as represented by the equation

- .

where

- is the semi-major axis
- is the semi-minor axis
- is the semi-latus rectum
- is the gravitational constant
- , are the two masses.