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Exoplanet transit depth and duration calculator

Estimate how much a planet dims its star when it passes in front, how long the transit lasts and how likely a random orbit is to produce transits.

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Transit depth

84 ppm

Under 100 ppm: Earth-size signal, needs space telescopes such as Kepler, TESS or PLATO

Transit duration (central transit)

13.1 h

Transit depth in percent
0.008386 %
Orbital distance
1 AU
Probability that a random orbit transits
0.465 %

The transit method

When a planet passes in front of its star as seen from Earth, it blocks a tiny fraction of the starlight. Space telescopes such as Kepler and TESS have found thousands of exoplanets by watching for these regular dips in brightness.

Transit depth

The fraction of light blocked is roughly the ratio of the two disks’ areas:

Depth ≈ (Rp ÷ R)²*

where Rp is the planet’s radius and R* the star’s. Depth is often expressed in parts per million (ppm).

  • Earth crossing the Sun: about 84 ppm (0.0084%).
  • Jupiter crossing the Sun: about 1%.
  • An Earth-size planet around a small red dwarf: several thousand ppm, much easier to see.

Transit duration

For a planet crossing the center of the star’s disk, the transit lasts about:

T ≈ (P ÷ π) × arcsin((R + Rp) ÷ a)*

where P is the orbital period and a the orbital distance, which Kepler’s third law gives from the period and the star’s mass: a (AU) = (M × P²)^(1/3), with P in years. Off-center transits are shorter.

Example: Earth seen from afar

An alien astronomer watching the Sun from the right direction would see Earth:

  • dim the Sun by 84 ppm;
  • for about 13 hours;
  • once a year.

That is why detecting a true Earth twin needs extremely precise, long space-based observations.

Transit probability

A transit only happens if the orbit is nearly edge-on to us. For random orientations, the probability is about R ÷ a*:

  • Earth around the Sun: about 0.47%;
  • a hot Jupiter at 0.05 AU: about 10%.

So for every transiting planet found, many more around nearby stars go unseen.

What else transits reveal

  • Combined with radial-velocity measurements of the planet’s mass, the radius gives its density: rocky, water-rich or gaseous.
  • Starlight filtered through the planet’s atmosphere during transit reveals its composition, as JWST does for water, carbon dioxide and other molecules.
  • Variations in transit timing can reveal other, unseen planets in the system.

Real light curves also depend on limb darkening, star spots and the impact parameter, which professional fits take into account.

Frequently asked questions

What is transit depth?

It is the fractional dip in starlight as a planet crosses its star, equal to (planet radius / star radius)². An Earth around the Sun gives about 84 parts per million.

How long does a transit last?

For a central transit on a circular orbit, roughly the period times the star's diameter divided by the orbit circumference. Earth seen from afar would transit for about 13 hours.

What is the transit probability?

A random observer sees transits only if the orbit is nearly edge-on. The chance is about star radius divided by orbital distance, roughly 0.5 percent for Earth.

Why are big planets easier to detect?

Depth scales with the square of the radius, so a Jupiter (about 1 percent dip) is around 100 times easier to see than an Earth.

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Results are estimates provided for information purposes. They do not replace professional advice.