bolometric magnitude

When referring to total energy output, the proper term is bolometric magnitude.

The Sun's absolute bolometric magnitude is set arbitrarily, usually at 4.75.

The difference in bolometric magnitude is related to the luminosity ratio according to:

The measure of luminosity is "bolometric magnitude", the total power output across all wavelengths.

If it is necessary to talk about the total power output across all wavelengths, that is called bolometric magnitude.

Bolometric magnitude is luminosity expressed in magnitude units; it takes into account energy radiated at all wavelengths, whether observed or not.

The bolometric magnitude can be computed from the visual magnitude plus a bolometric correction, .

The bolometric correction scale is set by the absolute magnitude of the Sun and an adopted bolometric magnitude for the Sun.

A kinematic distance of 5.4 kpc and a bolometric magnitude of -9.4 put HR Car among the most luminous stars of the galaxy.

In practice bolometric magnitudes are measured by taking measurements at certain wavelengths and constructing a model of the total spectrum that is most likely to match those measurements.

The star, designated M31-RV, reached the absolute bolometric magnitude of 9.95 at maximum (corresponding a luminosity of 0.75 million times solar) before dimming beyond detectability.

The 1999 IAU statements define that absolute bolometric magnitude zero correlates to a bolometric luminosity of 3.055e28 Watts.

Other metrics are absolute magnitude, which is an object's intrinsic brightness at visible wavelengths, irrespective of distance, while bolometric magnitude is the total power output across all wavelengths.

Likely a luminous blue variable (LBV), it has an absolute bolometric magnitude of 10.9 (1.8 million solar units), making it one of the most luminous stars known.

Its visual magnitude implies an overluminous bolometric magnitude; SN 1920A has since been classified as anomalous and is believed to be the result of "a completely different explosion mechanism."

In astronomy, a bolometric correction is a correction that must be made to the absolute magnitude of an object in order to convert an object's visible magnitude to its bolometric magnitude.

Bolometric magnitude corresponds to luminosity, expressed in magnitude units; that is, after taking into account all electromagnetic wavelengths, including those unobserved due to instrumental pass-band, the Earth's atmospheric absorption, or extinction by interstellar dust.

When converting luminosity or absolute bolometric magnitude to apparent or absolute visual magnitude, one requires a bolometric correction, which may or may not come from the same source as the color-temperature relation.

Combining its absolute visible brightness, its infrared radiation, and correcting for its interstellar extinction gives a luminosity of around 350,000 solar luminosities (bolometric magnitude about 9.1), making it one of the most luminous stars known.

This particular luminosity was selected as the zero-point for the absolute bolometric magnitude scale so that the Sun's luminosity (3.842e26 Watts) would correspond to absolute bolometric magnitude 4.75 (the value that was most commonly used by most astronomers).