Crab pulsar spin-down power
Crab pulsar spin-down power is the rate at which the Crab pulsar loses rotational energy, emitting it as radiation and particles.
How big is it?
4.6 × 10¹⁹ TW · spin-down power
Spin-down power · derived estimate
A little perspective
Crab pulsar spin-down power vs Eddington luminosity of a solar-mass object: 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
Crab pulsar spin-down power is the rate at which the Crab pulsar loses rotational energy, emitting it as radiation and particles.
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.
Measurements, assumptions & sources +
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.
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.
Use the visual comparison to explore its scale, then check the measurements and sources.
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Why this measurement?
Why we use 4.6 × 10¹⁹ TW
We compare the spin-down power of the Crab Pulsar. The measurement is labelled derived estimate. Check the source notes for its basis.
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.
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 |
|---|---|---|---|
| 4.6 × 10¹⁹ TW | Not recorded | derived estimate |
Around this scale
Explore nearby values.
Compare examples with lower, similar and higher values. Each card names the measurement being compared.
Nearest lower valuePower and outputEddington luminosity of a solar-mass object1.3 × 10¹⁹ TWPowerThe 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.
Nearest higher valuePower and outputAndromeda galaxy stellar luminosity1 × 10²⁵ TWRepresentative stellar luminosityAndromeda galaxy stellar luminosity is the total power emitted as starlight by all the stars in the Andromeda galaxy.Sources and method
Want to check the number?
The source records and measurement method remain available for inspection.
- Fermi-LAT Collaboration — Fermi-LAT observations of the Crab nebula and pulsarReports Crab pulsar spin-down power of 4.6 × 10^38 erg s−1; this rotational energy-loss rate is inferred from pulsar timing and depends on the assumed neutron-star moment of inertia.
There’s always another scale
Follow your curiosity.
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