Orbital Velocity Calculator: Vis-Viva, Escape Velocity & Period

Orbital Velocity Calculator

Circular & elliptical (vis-viva) · escape velocity · period

Central Body

Pick a body to pre-fill μ and radius, or choose Custom and type any μ for another planet, moon or hypothetical body — both fields always stay editable.

Orbit Position

Elliptical Orbit

Both are altitudes above the surface. Vis-viva gives the true velocity at each point — fastest at perigee, slowest at apogee.

Result

Pick a central body and orbit to get the orbital velocity, escape velocity for comparison, and the orbital period — or switch to elliptical mode for vis-viva velocities at perigee and apogee

These are ideal two-body Keplerian results: they assume a point-mass central body and ignore atmospheric drag, oblateness (J2), third-body perturbations and relativistic effects. Real low orbits decay from drag, and precise mission design needs a full propagator. Orbital radius must exceed the body radius — an orbit inside the surface is unphysical. The geostationary reference applies to Earth only. Escape velocity is the speed needed to reach infinity with zero residual velocity from that radius, ignoring other bodies. For study and preliminary analysis, not flight dynamics.


Orbital Velocity Calculator: Circular and Elliptical Vis-Viva, Escape Velocity and Period

Most orbital velocity tools only handle the simple circular case, but a real satellite orbit is usually elliptical, moving fastest at perigee and slowest at apogee and a plain circular formula can’t capture that. This vis-viva calculator does both. It computes circular orbital velocity around Earth, the Moon, Mars, or the Sun with gravitational parameters pre-filled or any custom body via a directly editable μ and its elliptical mode takes your apogee and perigee altitudes and returns the true velocity at both points using the full vis-viva equation. Every result comes with a built-in escape velocity calculator reading alongside for direct comparison and an orbital period calculator using Kepler’s third law, shown in minutes, hours or days as appropriate, plus a geostationary quick-reference for a familiar earth benchmark.


How to Use

This tool has two tabs: Circular Orbit and Elliptical (Vis-Viva).

Step 1: Setting up your central body (shared across both modes)

  • Select a Body from the dropdown, Earth, Moon, Mars, and the Sun are included, to pre-fill the Gravitational Parameter μ and Body Radius. Both fields always stay fully editable, so you can select Custom and type any μ for another planet, moon or hypothetical body entirely.

Step 2: Using Circular Orbit mode

  • Enter your orbit Value and select whether it should be Interpreted as an Altitude above surface or an absolute Radius from centre.
  • Tap Calculate Circular Orbit. The result shows orbital velocity, escape velocity at that same radius for comparison, and the orbital period.
  • Alternatively, tap Load Geostationary (Earth) to instantly load the standard ~35,786 km geostationary altitude and see its familiar orbital velocity and 24-hour-class period.

Step 3: Using Elliptical (Vis-Viva) mode

  • Switch to the Elliptical (Vis-Viva) tab. Enter your Perigee Altitude and Apogee Altitude, both measured above the body’s surface.
  • Tap Calculate Elliptical Orbit. Instead of assuming a circular path, tool applies the full vis-viva equation to give you the true velocity at both perigee, where the satellite moves fastest and apogee, where it moves slowest.

Step 4: Exporting your result

  • Use Print / PDF for a clean printable copy or Copy to paste the figures elsewhere.

Key Features

  • Circular orbital velocity for Earth, Moon, Mars, or the Sun, with a directly editable μ for any custom body
  • Full vis-viva elliptical mode, giving true velocity at both perigee and apogee, not just an averaged circular estimate
  • Escape velocity shown alongside every result for direct comparison at the same radius
  • Orbital period from Kepler’s third law, displayed in minutes, hours or days depending on scale
  • Geostationary quick-reference button, instantly loading Earth’s ~35,786 km GEO altitude
  • Accepts orbit position as either altitude above the surface or absolute radius from the centre
  • Export as PDF or copy the result.

Formula / Logic Used

Circular Orbital Velocity

v=μrv = \sqrt{\frac{\mu}{r}}

Where μ\mu is the central body’s gravitational parameter and rr is the orbital radius, measured from the body’s centre.

Vis-Viva Equation (Elliptical Orbit)

v=μ(2r1a),a=rapo+rperi2v = \sqrt{\mu\left(\frac{2}{r} – \frac{1}{a}\right)}, \qquad a = \frac{r_{apo} + r_{peri}}{2}

Evaluating this at r=rperir = r_{peri}​ gives the fastest velocity in the orbit and at r=rapor = r_{apo}​ gives the slowest, since aa, the semi-major axis, stays fixed for the whole ellipse.

Escape Velocity

vesc=2μrv_{esc} = \sqrt{\frac{2\mu}{r}}

Escape velocity at any given radius is always √2 times the circular orbital velocity at that same radius.

Orbital Period (Kepler’s Third Law)

T=2πr3μ (circular),T=2πa3μ (elliptical)T = 2\pi\sqrt{\frac{r^3}{\mu}} \ \text{(circular)}, \qquad T = 2\pi\sqrt{\frac{a^3}{\mu}} \ \text{(elliptical)}


Who Should Use This Tool

Aerospace engineering and physics students learning orbital mechanics, the vis-viva equation and Kepler’s laws for a spaceflight dynamics or astrodynamics course. Also useful for space enthusiasts and hobbyist satellite trackers wanting a quick, correct velocity and period estimate for a given orbit.


Frequently Asked Questions (FAQs)

1. How do I calculate the orbital velocity of a satellite in a circular orbit?

Take the square root of the central body’s gravitational parameter divided by the orbital radius, measured from the body’s centre, not from its surface. This tool calculates it instantly once you select a body and enter your altitude or radius, automatically adding the body’s radius when you enter an altitude.

2. Why is the vis-viva equation needed instead of the simple circular formula?

A real elliptical orbit doesn’t move at a constant speed, it moves fastest at perigee (closest approach) and slowest at apogee (farthest point) and the simple circular velocity formula can not capture that variation. This tool’s elliptical mode applies the full vis-viva equation, which correctly accounts for both the current radius and the orbit’s semi-major axis together.

3. What is the relationship between orbital velocity and escape velocity?

Escape velocity at any given radius is always exactly the square root of 2 times the circular orbital velocity at that same radius, since escaping to infinity requires overcoming twice the kinetic energy of a stable circular orbit. This tool shows both figures together for every calculation so you can see this relationship directly.

4. Why is the geostationary orbit altitude the same for every satellite at that height?

A geostationary orbit is defined by matching the satellite’s orbital period exactly to Earth’s rotational period, which for a circular orbit corresponds to one specific altitude, roughly 35,786 km, regardless of the satellite’s mass. This tool’s dedicated geostationary reference button loads this exact altitude instantly for Earth.

5. Are these orbital calculations accurate enough for real mission planning?

No, these are ideal two-body Keplerian results that assume a point-mass central body and ignore atmospheric drag, Earth’s oblateness, third-body gravitational perturbations, and relativistic effects, all of which matter for real spacecraft. This tool is built for learning orbital mechanics fundamentals and preliminary estimation, real mission design needs a full numerical propagator accounting for these additional effects.


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