It really depends on the units used. Sometimes the Sun is used as a comparison for the brightness of other stars, or even galaxies - in this case, the Sun's luminosity is arbitrarily defined as 1, and a star that is 10 times brighter will have luminosity 10, for example. However, if you use other units, for example watts, you get quite different numbers (3.846×1026 watts for the Sun, according to the Wikipedia).
Deneb has a luminosity (apparent magnitude) of 1.25. However, in bolometric luminosity (solar units) Deneb is 54,000, whereas our Sun is 1.
The luminosity of the Sun is approximately 3.8 x 10^26 watts, which means it is emitting this amount of energy every second. This energy output is generated through nuclear fusion reactions in the Sun's core.
The Sun is the main basis for many stellar parameters. A far as luminosity goes - it is 1.
V
No.
A solar luminosity is equal to the current luminosity of the Sun, which is 3.839 × 1026 W, or 3.839 × 1033 erg/s.So dividing one solar luminosity with the Suns luminosity gives 1.Also it is a lot easier talking about a luminosity of 1 rather than 3.838 x 1026 W, the same way astronomers use 1 AU to mean 150,000,000km.
Deneb has a luminosity (apparent magnitude) of 1.25. However, in bolometric luminosity (solar units) Deneb is 54,000, whereas our Sun is 1.
The luminosity of the Sun is approximately 3.8 x 10^26 watts, which means it is emitting this amount of energy every second. This energy output is generated through nuclear fusion reactions in the Sun's core.
A star's luminosity is measured according to the relevance to the sun. Basically for example, if a star is 8,300 degrees Celsius and has a luminosity of 0.001; the luminosity is compared to the sun.
The Sun is the main basis for many stellar parameters. A far as luminosity goes - it is 1.
To find the mass corresponding to a luminosity of 3160 times that of the Sun, we can use the mass-luminosity relationship for main-sequence stars, which states that luminosity (L) is proportional to mass (M) raised to approximately 3.5 power (L ∝ M^3.5). Rearranging this gives us M ≈ (L/L_sun)^(1/3.5), where L_sun is the luminosity of the Sun. Plugging in 3160 for luminosity, the mass would be roughly 15.5 times the mass of the Sun.
V
The main star in the Polaris system has a luminosity which is 2500 times that of the Sun.
The Sun is classified as a G2V star in the Hertzsprung-Russell diagram, where "G2" indicates its surface temperature and spectral characteristics, and "V" denotes its luminosity class as a main-sequence star. This classification reflects that the Sun is a stable, hydrogen-burning star that is currently in the main sequence phase of its stellar evolution. Its luminosity is approximately 1 solar luminosity (L☉), serving as a standard reference for comparing other stars.
Sirius
No.
3.826x1026 is the luminosity, in Joules/second, of our sun.