(difference between an object's bolometric and visible magnitudes)
Bolometric correction is
a difference in magnitude applied to stars to determine
their bolometric magnitude from their visible magnitude.
It varies by type of star, e.g., spectral type, and is
largest for stars much hotter or cooler than the Sun because
the EMR from stars of the Sun's temperature
is centered around visible light.
Some bolometric correction examples:
|O3 star||-4.3 for a main sequence star||-4.2 for a giant|
|G0 star||-0.10 for a main sequence star||-0.13 for a giant|
|M0 star ||-1.21 for a main sequence star||-1.28 for a giant|
Referenced by pages:
bolometric magnitude (Mbol)