Saha equation describes the ionization state of a gas in thermal equilibrium, relating temperature and pressure to the degree of ionization.In 1920, Indian physicist Meghnad Saha combined thermodynamics and quantum mechanics to explain the solar spectrum. The essence is simple: in collisions within a hot gas, atoms can become ionized, i.e., lose electrons. The equation relates the concentrations of neutral atoms, ions, and electrons to temperature and pressure. It's like a balance between lotteries and prizes: the more expensive the prize (ionization energy), the fewer 'customers' (ions). The equation became the key to deciphering starlight.
Meghnad Saha, an Indian physicist and astrophysicist, derived the equation in 1920 while working on the theory of stellar atmospheres. He developed the ideas of Arthur Stanley Eddington and Karl Schwarzschild. Later, Irving Langmuir generalized the equation to multi-electron ionization, and Cecilia Payne-Gaposchkin used it to analyze the solar composition, proving the dominance of hydrogen.
It is applied in stellar spectroscopy: from the observed distribution of absorption lines of different ions, the electron temperature and density in stellar atmospheres are determined. Limitations: it assumes local thermodynamic equilibrium, which breaks down in rarefied nebulae or in the presence of strong non-thermal radiation sources.
Astrophysicists determine the temperature and chemical composition of stars from absorption lines in spectra, using ionization balance.
Using the Saha equation, it was first correctly determined that the Sun is mostly hydrogen, not iron, as previously thought.
| w | variable | equation of state parameter — equation of state parameter |
| P | variable | pressure — pressure pascal |
| ρ | variable | energy density — energy density joule per cubic metre |
| \dot{n}_{\text{ion}} | variable | ionization rate per unit volume — ionization rate metre per second per cubic metre |
| L | variable | line luminosity — luminosity watt |
| R | variable | emission coefficient — emission coefficient watt per cubic metre per steradian |
| c | variable | speed of light — speed of light metre per second |
| f_{\text{esc}} | variable | escape fraction of ionizing photons — escape fraction |
| p | variable | Pressure of the gas — pressure pascal |
| ρ | variable | Mass density of the gas — mass density kilogram per metre cubed |
| T | variable | Absolute temperature — temperature kelvin |
| μ | variable | Mean molar mass of the gas mixture — molar mass kilogram per mole |
| R | constant | Universal gas constant relating energy scale to temperature — gas constant = 8.314462618 joule per mole kelvin |
| M(<r) | variable | mass enclosed within radius r — mass kilogram |
| r | variable | radial distance from the center — radius metre |
| P | variable | pressure — pressure pascal |
| G | constant | constant of proportionality in Newton's law of universal gravitation — gravitational constant = 6.67430e-11 cubic metre per kilogram per second squared |
| dP/dr | operator | derivative of pressure with respect to radius — radial derivative |



