apoapsis , także: apoapse

The point farthest from the attracting body is called the apoapsis.

A line drawn from periapsis to apoapsis is the line-of-apsides.

This slowing caused the spacecraft to lose altitude on its next pass through the orbit's apoapsis.

The angular rate is faster nearer periapsis and slower near apoapsis.

It is the inverse of the apoapsis distance (maximum distance).

Still an ellipse, this time around Jupiter itself, and the new apoapsis continued to climb, if languidly.

For the most efficient example mentioned above, targeting an inclination at apoapsis also changes the argument of periapsis.

The eccentricity of 0.7512 gives it an apoapsis that is seven times its periapsis distance from Neptune.

A straight line drawn through the periapsis and apoapsis is the line of apsides.

The signal looked like a strong enhancement of the forward-scattering at the wavelength 3.6 cm near ring's apoapsis.

There is no periapsis or apoapsis.

Other orbital parameters can be computed from the Keplerian elements such as the period, apoapsis, and periapsis.

The semi-major axis a is the average of the radius at apoapsis and periapsis:

Periapsis and apoapsis (or apapsis) are equivalent alternatives.

However, maximum efficiency of inclination changes are achieved at apoapsis, (or apogee), where orbital velocity is the lowest.

With increasing release height the orbit would become less eccentric as both periapsis and apoapsis increase, becoming circular at geostationary level.

Semimajor axis () - the sum of the periapsis and apoapsis distances divided by two.

In other cases, boosting up to a relatively high altitude apoapsis gives low speed before performing the plane change and this can give lower total delta-v.

It would take an hour for the apoapsis to climb out of Jovian space, and another sixty before Louis Pasteur did so herself.

Each orbit consisted of an 80-minute lunar mapping phase near periapsis and 139 minutes of downlink at apoapsis.

The radially integrated brightness of the ε ring is highest near apoapsis and lowest near periapsis.

Let 2a be the distance measured along the apse line from periapsis P to apoapsis A, as illustrated in the equation below:

The eccentricity of an elliptical orbit can also be used to obtain the ratio of the periapsis to the apoapsis:

The point where the satellite is farthest from Earth is called the apogee, apoapsis, or sometimes apifocus or apocentron.

Orbital periods vary according to the sum of apoapsis and periapsis, and for the CSM were about two hours.