Linked from

The 20 pages that link to Eddington luminosity, each with the reason it gives.

• Active galactic nucleusRelated: It provides a benchmark for comparing an active nucleus’s luminosity with its black-hole mass.

• QuasarRelated: It helps explain how a quasar’s brightness constrains its black hole’s growth.

• Supermassive black holeRelated: It constrains steady growth, sharpening the puzzle of how some early black holes became massive so quickly.

• Stellar massRelated: It helps limit how luminous and massive a stable star can become.

• Massive starRelated: It helps explain why extreme luminosity constrains the masses and stability of massive stars.

• X-ray binaryRelated: It provides a benchmark for interpreting how brightly an X-ray binary accretes.

• Stellar mass lossRelated: Stars near this limit may launch powerful outflows, but the threshold depends on opacity and structure.

• Mass–luminosity relationRelated: Near this limit, very massive stars cannot follow an unrestricted luminosity increase with mass.

• Luminous blue variableRelated: Approaching this limit can make a luminous blue variable’s outer layers unstable.

• Ultraluminous infrared galaxyRelated: It provides a benchmark for whether compact star-forming regions approach radiation-pressure limits.

• Blue supergiantRelated: It helps explain why the most luminous stars lose mass so forcefully.

• R136Related: Comparing R136’s brightest stars with this limit helps constrain their masses and structure.

• HypergiantRelated: Approaching this limit helps explain why hypergiants shed matter so rapidly.

• LBV 1806−20Related: Near this limit, radiation pressure can destabilize a massive star’s outer layers.