unit of radiant flux in astronomy
Evolution of the solar luminosity, radius and effective temperature compared to the present-day Sun. After Ribas (2010) The solar luminosity (L☉) is a unit of radiant flux (power emitted in the form of photons) conventionally used by astronomers to measure the luminosity of stars, galaxies and other celestial objects in terms of the output of the Sun.
One nominal solar luminosity is defined by the International Astronomical Union to be 3.828×10 W. This corresponds almost exactly to a bolometric absolute magnitude of +4.74.
Discovered by embedding cosine similarity (sentence-transformers MiniLM, 384-dim).