Eddington luminosity of a solar-mass object
The Eddington luminosity of a solar-mass object is the theoretical maximum brightness a star with the Sun's mass can achieve before radiation pressure overcomes gravity.
How big is it?
1.3 × 10¹⁹ TW · power
Power · theoretical
A little perspective
Eddington luminosity of a solar-mass object vs Crab pulsar spin-down power: power comparison
The spin-down power of the Crab Pulsar is about 3.54 times the Eddington luminosity of a solar-mass object.
ENERGY EACH SECOND
The Eddington luminosity of a solar-mass object is the theoretical maximum brightness a star with the Sun's mass can achieve before radiation pressure overcomes gravity.
Crab pulsar spin-down power is the rate at which the Crab pulsar loses rotational energy, emitting it as radiation and particles.
Measurements, assumptions & sources +
Eddington luminosity of a solar-mass object
Power: 1.3 × 10¹⁹ TW; theoretical.
The Eddington luminosity is a theoretical force-balance threshold, not an observed stellar brightness. This rounded one-solar-mass value assumes pure ionized-hydrogen electron-scattering opacity (about 0.4 cm²/g).
Theoretical Eddington value for one solar mass using pure ionized-hydrogen electron-scattering opacity (about 0.4 cm²/g); other opacity and composition change the result.
Monash University — Astrophysics I: Stars and Stellar Evolution, Lecture 25
The marked power is calibrated. Unmeasured illustration details are representative.
Crab pulsar spin-down power
Spin-down power: 4.6 × 10¹⁹ TW; derived estimate.
The Crab pulsar's rotational energy-loss rate is inferred from its spin-down using a canonical neutron-star moment of inertia; the quoted value is a rounded literature estimate, not its bolometric output.
A timing-derived rotational energy-loss estimate using a canonical neutron-star moment of inertia; it is not the pulsar's directly measured total emitted luminosity.
Fermi-LAT Collaboration — Fermi-LAT observations of the Crab nebula and pulsar
The marked spin-down power is calibrated. Unmeasured illustration details are representative.
Use the visual comparison to explore its scale, then check the measurements and sources.
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Why this measurement?
Why we use 1.3 × 10¹⁹ TW
We compare the Eddington luminosity of a solar-mass object. This is a theoretical value calculated under stated physical assumptions, not a direct observation.
The Eddington luminosity is a theoretical force-balance threshold, not an observed stellar brightness. This rounded one-solar-mass value assumes pure ionized-hydrogen electron-scattering opacity (about 0.4 cm²/g).
Theoretical Eddington value for one solar mass using pure ionized-hydrogen electron-scattering opacity (about 0.4 cm²/g); other opacity and composition change the result.
The picture identifies the subject; the diagram compares the recorded values. How calibrated comparisons work →
Recorded properties
Dimensions and measurements
| Property | Selected value | Recorded range | Basis |
|---|---|---|---|
| 1.3 × 10¹⁹ TW | Not recorded | theoretical |
Around this scale
Explore nearby values.
Compare examples with lower, similar and higher values. Each card names the measurement being compared.
Nearest lower valuePlanets, moons and spaceSun3.828 × 10¹⁴ TWLuminosityThe Sun is the star at the centre of the Solar System.Nearest higher valuePower and outputCrab pulsar spin-down power4.6 × 10¹⁹ TWSpin-down powerCrab pulsar spin-down power is the rate at which the Crab pulsar loses rotational energy, emitting it as radiation and particles.Sources and method
Want to check the number?
The source records and measurement method remain available for inspection.
- Monash University — Astrophysics I: Stars and Stellar Evolution, Lecture 25Derives the Eddington limit from radiation force balance. The canonical one-solar-mass value assumes pure ionized hydrogen, with electron-scattering opacity about 0.4 cm²/g; other composition changes it.
There’s always another scale
Follow your curiosity.
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