equation

Saha equation

Saha equation describes the ionization state of a gas in thermal equilibrium, relating temperature and pressure to the degree of ionization.
10 related articles · 4 formulas

Description

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.

History

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.

How it works

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.

In practice

Astrophysicists determine the temperature and chemical composition of stars from absorption lines in spectra, using ionization balance.

Fun fact

Using the Saha equation, it was first correctly determined that the Sun is mostly hydrogen, not iron, as previously thought.

Concept graph →

Formulas

$$w = \frac{P}{\rho}$$
Relates pressure to energy density in cosmology.
What is in the formula
wvariableequation of state parameter — equation of state parameter
Pvariablepressure — pressure pascal
ρvariableenergy density — energy density joule per cubic metre
φ=p/\varepsilon · 2601.02980v1
w=-1 · 2601.06656v1
w=-1 · 2605.20060
w=\frac{p}{ρ} · 2605.13705v1
$$\dot{n}_{\text{ion}} = \frac{L}{R \, c \, (1-f_{\text{esc}})}$$
Ionization rate equals line luminosity divided by escape fraction and emission coefficient.
What is in the formula
\dot{n}_{\text{ion}}variableionization rate per unit volume — ionization rate metre per second per cubic metre
Lvariableline luminosity — luminosity watt
Rvariableemission coefficient — emission coefficient watt per cubic metre per steradian
cvariablespeed of light — speed of light metre per second
f_{\text{esc}}variableescape fraction of ionizing photons — escape fraction
\dot{n}_{{ion}}=\frac{l_{[{oiii}]+{h}β}}{rc_{{h}β}(1-f_{{esc}})} · 2606.05323v1
$$p = \frac{\rho R T}{\mu}$$
Pressure relates to density, temperature, and molar mass.
What is in the formula
pvariablePressure of the gas — pressure pascal
ρvariableMass density of the gas — mass density kilogram per metre cubed
TvariableAbsolute temperature — temperature kelvin
μvariableMean molar mass of the gas mixture — molar mass kilogram per mole
RconstantUniversal gas constant relating energy scale to temperature — gas constant = 8.314462618 joule per mole kelvin
p=ρ\frac{rt}{μ} · 2607.02691
$$M(<r) = -\frac{r^2}{G}\frac{dP}{dr}$$
Mass enclosed within radius r derived from pressure gradient under hydrostatic equilibrium.
What is in the formula
M(<r)variablemass enclosed within radius r — mass kilogram
rvariableradial distance from the center — radius metre
Pvariablepressure — pressure pascal
Gconstantconstant of proportionality in Newton's law of universal gravitation — gravitational constant = 6.67430e-11 cubic metre per kilogram per second squared
dP/droperatorderivative of pressure with respect to radius — radial derivative
m_{\rmhse}(<r)=-\frac{r^2}{g}\frac{dp}{dr}\frac{1}{n_g} · 2607.20721v1

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