Part of a series on
Astrodynamics
Orbital mechanics
Orbital elements Apsis Argument of periapsis Eccentricity Inclination Mean anomaly Orbital nodes Semi-major axis True anomaly
Types of two-body orbits by eccentricity Circular orbit Elliptic orbit Transfer orbit (Hohmann transfer orbit Bi-elliptic transfer orbit) Parabolic orbit Hyperbolic orbit Radial orbit Decaying orbit
Equations Dynamical friction Escape velocity Kepler's equation Kepler's laws of planetary motion Orbital period Orbital velocity Surface gravity Specific orbital energy Vis-viva equation
Celestial mechanics
Gravitational influences Barycenter Hill sphere Perturbations Sphere of influence
N-body orbits Lagrangian points (Halo orbits) Lissajous orbits Lyapunov orbits
Engineering and efficiency
Preflight engineering Mass ratio Payload fraction Propellant mass fraction Tsiolkovsky rocket equation
Efficiency measures Gravity assist Oberth effect
v t e

A circular orbit is an orbit with a fixed distance around the barycenter; that is, in the shape of a circle. In this case, not only the distance, but also the speed, angular speed, potential and kinetic energy are constant. There is no periapsis or apoapsis. This orbit has no radial version.

Listed below is a circular orbit in astrodynamics or celestial mechanics under standard assumptions. Here the centripetal force is the gravitational force, and the axis mentioned above is the line through the center of the central mass perpendicular to the orbital plane.

Circular acceleration

Transverse acceleration (perpendicular to velocity) causes change in direction. If it is constant in magnitude and changing in direction with the velocity, circular motion ensues. Taking two derivatives of the particle's coordinates with respect to time gives the centripetal acceleration

${\displaystyle a\,={\frac {v^{2)){r))\,={\omega ^{2)){r))$

where:

• ${\displaystyle v\,}$ is orbital velocity of orbiting body,
• ${\displaystyle r\,}$ is radius of the circle
• ${\displaystyle \omega \ }$ is angular speed, measured in radians per unit time.

The formula is dimensionless, describing a ratio true for all units of measure applied uniformly across the formula. If the numerical value of ${\displaystyle \mathbf {a} }$ is measured in meters per second per second, then the numerical values for ${\displaystyle v\,}$ will be in meters per second, ${\displaystyle r\,}$ in meters, and ${\displaystyle \omega \ }$ in radians per second.

Velocity

The speed (or the magnitude of velocity) relative to the central object is constant:^[1]: 30

${\displaystyle v={\sqrt {GM\! \over {r))}={\sqrt {\mu \over {r))))$

where:

• ${\displaystyle G}$, is the gravitational constant
• ${\displaystyle M}$, is the mass of both orbiting bodies ${\displaystyle (M_{1}+M_{2})}$, although in common practice, if the greater mass is significantly larger, the lesser mass is often neglected, with minimal change in the result.
• ${\displaystyle \mu =GM}$, is the standard gravitational parameter.

Equation of motion

The orbit equation in polar coordinates, which in general gives r in terms of θ, reduces to:^{[clarification needed][citation needed]}

${\displaystyle r=((h^{2)) \over {\mu ))}$

where:

• ${\displaystyle h=rv}$ is specific angular momentum of the orbiting body.

This is because ${\displaystyle \mu =rv^{2))$

Angular speed and orbital period

${\displaystyle \omega ^{2}r^{3}=\mu }$

Hence the orbital period (${\displaystyle T\,\!}$) can be computed as:^[1]: 28

${\displaystyle T=2\pi {\sqrt {r^{3} \over {\mu ))))$

Compare two proportional quantities, the free-fall time (time to fall to a point mass from rest)

${\displaystyle T_{\text{ff))={\frac {\pi }{2{\sqrt {2)))){\sqrt {r^{3} \over {\mu ))))$ (17.7% of the orbital period in a circular orbit)

and the time to fall to a point mass in a radial parabolic orbit

${\displaystyle T_{\text{par))={\frac {\sqrt {2)){3)){\sqrt {r^{3} \over {\mu ))))$ (7.5% of the orbital period in a circular orbit)

The fact that the formulas only differ by a constant factor is a priori clear from dimensional analysis.^{[citation needed]}

Energy

The specific orbital energy (${\displaystyle \epsilon \,}$) is negative, and

${\displaystyle \epsilon =-{v^{2} \over {2))}$

${\displaystyle \epsilon =-{\mu \over {2r))}$

Thus the virial theorem^[1]: 72 applies even without taking a time-average:^{[citation needed]}

• the kinetic energy of the system is equal to the absolute value of the total energy
• the potential energy of the system is equal to twice the total energy

The escape velocity from any distance is √2 times the speed in a circular orbit at that distance: the kinetic energy is twice as much, hence the total energy is zero.^{[citation needed]}

Delta-v to reach a circular orbit

Maneuvering into a large circular orbit, e.g. a geostationary orbit, requires a larger delta-v than an escape orbit, although the latter implies getting arbitrarily far away and having more energy than needed for the orbital speed of the circular orbit. It is also a matter of maneuvering into the orbit. See also Hohmann transfer orbit.

Orbital velocity in general relativity

In Schwarzschild metric, the orbital velocity for a circular orbit with radius ${\displaystyle r}$ is given by the following formula:

${\displaystyle v={\sqrt {\frac {GM}{r-r_{S))))}$

where ${\displaystyle \scriptstyle r_{S}={\frac {2GM}{c^{2))))$ is the Schwarzschild radius of the central body.

Derivation

For the sake of convenience, the derivation will be written in units in which ${\displaystyle \scriptstyle c=G=1}$.

The four-velocity of a body on a circular orbit is given by:

${\displaystyle u^{\mu }=({\dot {t)),0,0,{\dot {\phi )))}$

(${\displaystyle \scriptstyle r}$ is constant on a circular orbit, and the coordinates can be chosen so that ${\displaystyle \scriptstyle \theta ={\frac {\pi }{2))}$). The dot above a variable denotes derivation with respect to proper time ${\displaystyle \scriptstyle \tau }$.

For a massive particle, the components of the four-velocity satisfy the following equation:

${\displaystyle \left(1-{\frac {2M}{r))\right){\dot {t))^{2}-r^{2}{\dot {\phi ))^{2}=1}$

We use the geodesic equation:

${\displaystyle {\ddot {x))^{\mu }+\Gamma _{\nu \sigma }^{\mu }{\dot {x))^{\nu }{\dot {x))^{\sigma }=0}$

The only nontrivial equation is the one for ${\displaystyle \scriptstyle \mu =r}$. It gives:

${\displaystyle {\frac {M}{r^{2))}\left(1-{\frac {2M}{r))\right){\dot {t))^{2}-r\left(1-{\frac {2M}{r))\right){\dot {\phi ))^{2}=0}$

From this, we get:

${\displaystyle {\dot {\phi ))^{2}={\frac {M}{r^{3))}{\dot {t))^{2))$

Substituting this into the equation for a massive particle gives:

${\displaystyle \left(1-{\frac {2M}{r))\right){\dot {t))^{2}-{\frac {M}{r)){\dot {t))^{2}=1}$

Hence:

${\displaystyle {\dot {t))^{2}={\frac {r}{r-3M))}$

Assume we have an observer at radius ${\displaystyle \scriptstyle r}$, who is not moving with respect to the central body, that is, their four-velocity is proportional to the vector ${\displaystyle \scriptstyle \partial _{t))$. The normalization condition implies that it is equal to:

${\displaystyle v^{\mu }=\left({\sqrt {\frac {r}{r-2M))},0,0,0\right)}$

The dot product of the four-velocities of the observer and the orbiting body equals the gamma factor for the orbiting body relative to the observer, hence:

${\displaystyle \gamma =g_{\mu \nu }u^{\mu }v^{\nu }=\left(1-{\frac {2M}{r))\right){\sqrt {\frac {r}{r-3M))}{\sqrt {\frac {r}{r-2M))}={\sqrt {\frac {r-2M}{r-3M))))$

This gives the velocity:

${\displaystyle v={\sqrt {\frac {M}{r-2M))))$

Or, in SI units:

${\displaystyle v={\sqrt {\frac {GM}{r-r_{S))))}$