Photometry Simulator

Exoplanet Transit Hunter

Model Kepler & TESS transit light curve dips. Adjust host star classification, planetary radius, and orbital geometry to observe parts-per-million photometric variation.

Photometric Light Curve Laboratory

Exoplanet Transit Light Curve & Radius Estimator

Simulate Kepler & TESS transit depth (ΔF/F ≈ (R_p / R_★)²) and calculate planetary volumetric classification.

Planet Radius (R_⊕)2.40 Earths

Sub-Neptune / Hycean

Host Star Radius (R_☉)1.00 Sun

G-Type Sun-like Star

Orbital Period (P)12.5 Days

Semi-major: ~0.105 AU

Impact Parameter (b)0.20

Transit Latitude Cross-section

Photometric Light Curve Model

Transit Depth: 483 ppm (0.0483%)Duration: ~4.2 Hours

Flux = 1.0000 (Out of Transit)Relative Brightness Normalized

Ingress (T1)Central Transit (T_mid)Egress (T4)

Transit Depth

483.0 ppm

Radius Ratio (Rp/R★)

0.0220

Orbital Distance

0.105 AU

Detection Feasibility

TESS / Ground Telescopes

Transit Depth Formulation

For a spherical planet crossing a uniform stellar disk, the fraction of occulted starlight (transit depth $δ$) equals the geometric ratio of their projected surface areas:

δ = (R_p / R_★)²

An Earth-sized planet transiting a Sun-like star produces a tiny dip of only ~84 parts per million (0.0084%), requiring high-precision space telescopes like Kepler and PLATO.

Habitable Zone Boundaries

The circumstellar habitable zone (Goldilocks Zone) is the orbital shell where incident stellar flux permits liquid water to persist on a planet's surface. For M-dwarf stars, this zone lies very close (0.02 to 0.2 AU), causing tidal locking; for G-type stars, it spans roughly 0.95 to 1.4 AU.