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Luminosity Calculator

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What is luminosity?Luminosity equationAbsolute and apparent magnitudeCalculating luminosity: an exampleFAQs

This luminosity calculator is a handy tool that allows you to calculate the energy emitted by stars and how bright they appear when seen from Earth.

Thanks to this calculator, you will also be able to determine the absolute and apparent magnitudes of stars.

But that's not all – we will also provide you with a handy luminosity equation that will make comparing any two stars a piece of cake!

What is luminosity?

Luminosity is a measure of the energy radiated by an object, for example, a star or a galaxy. For the stars of the main sequence, luminosity is directly related to their temperature – the hotter a star, the more luminous it is. On the other hand, cooler stars emit less energy – hence, it's more challenging to spot them in the night sky.

Luminosity equation

We can derive the formula for stellar luminosity directly from the Stefan-Boltzmann law. This law states that for a black body, the energy radiated per unit time is equal to:

P=σAT4\small P = \sigma A T^4


  • σ\sigma – Stefan Boltzmann constant, equal to 5.670367 × 10-8W/(m2 K4);
  • AA – Surface area of the body (equal to 4πR24\pi R^2 for spherical objects); and
  • TT – Temperature of the body, expressed in Kelvins.

Visit our Stefan Boltzmann law calculator to learn more.

Our luminosity calculator uses a simplified version of this formula. Instead of calculating the energy as an arbitrary value, we can compare any star to the Sun. Then, after canceling out the constants, we arrive at the luminosity equation:

LL=(RR)2(TT)4\small \frac{L}{L_{\bigodot}} = \left(\frac{R}{R_{\bigodot}}\right)^2\left(\frac{T}{T_{\bigodot}}\right)^4


  • LL – Luminosity of the star;
  • RR – Star's radius;
  • TT – Star's temperature, measured in kelvins;
  • LL_{\bigodot} – Luminosity of the Sun, equal to 3.828 × 10²⁶ W;
  • RR_{\bigodot} – Sun's radius, equal to 695,700 km; and
  • TT_{\bigodot} – Temperature of the Sun, equal to 5778 K.

Absolute and apparent magnitude

You can also use this tool as an absolute magnitude calculator. Absolute magnitude is a different way to measure luminosity. Instead of expressing it in watts, it can be shown on a logarithmic scale.

The lower the absolute magnitude, the more luminous the star is - some very bright stars can even have negative magnitudes! For example, the absolute magnitude of the Sun is equal to 4.74, and of Bellatrix to −2.78.

Absolute magnitude and luminosity are related to the formula:

M=2.5log10 ⁣(LL0)\small M = -2.5 \log_{10}\!\left(\frac{L}{L_0}\right)


  • MM – Absolute magnitude of the star; and
  • L0L_0 – Zero-point luminosity, equal to 3.0128 × 10²⁸ W.

Apparent magnitude, on the other hand, is a measure of brightness when the star is seen from Earth – hence, it takes into account the distance between the star and the Earth. You can find it with the apparent magnitude calculator, using the following equation:

m=M5+5log10(D)\small m = M - 5 + 5 \log_{10}(D)


  • mm – Apparent magnitude of the star; and
  • DD – Distance between the star and Earth, measured in parsecs.

The absolute magnitude is defined as the apparent magnitude of an object seen from a distance of 10 parsecs. It means that for D = 10 parsecs, the apparent and absolute magnitudes are equal in value.

Calculating luminosity: an example

Let's analyze Sun with this luminosity calculator to investigate its absolute and apparent magnitude.

  1. Input the radius and temperature of the Sun into the calculator. The radius equals R=695,700 kmR_{\bigodot} = \text{695,700 km}, and the temperature is T=5778 KT_{\bigodot} = 5778\ \text K.

  2. The luminosity calculator will automatically find the luminosity of the Sun. It is equal to 3.828 × 10²⁶ W.

  3. To determine the absolute magnitude of the Sun, you can use the following equation:

M=2.5log10(LL0)=2.5log10(3.828×1026L0)=4.74\footnotesize \quad \begin{align*} M &= -2.5 \log_{10}\!\left(\frac{L}{L_0}\right)\\[1.5em] &= -2.5 \log_{10}\!\left(\frac{3.828\times 10^{26}}{L_0}\right)\\ &= 4.74 \end{align*}
  1. Last but not least, you can find the apparent magnitude of the Sun. The distance between the Earth and Sun equals 4.848 × 10⁻⁶ parsecs. After putting this value in the apparent magnitude formula, you will obtain
m=M5+5log10(D)=4.745+5log10(4.848×106)=26.83\footnotesize \quad \begin{align*} m &= M - 5 + 5 \log_{10}(D)\\ &= 4.74 - 5 + 5 \log_{10}(4.848\!\times\!10^{-6})\\ &= -26.83 \end{align*}

The apparent magnitude of the Sun is equal to -26.83.

💡 Similar to luminosity, radiance is another way to measure an object's brightness. Check our laser brightness calculator to learn more about it!


What is luminosity?

Luminosity, in astronomy, is a measure of the total power emitted by a light-emitting object, particularly by a star. The luminosity depends uniquely on the size and surface temperature of the object, and it's measured in multiples of the Joule per second or in watts. However, as these values can grow pretty big, we often express the luminosity as a multiple of the Sun's luminosity (L☉).

What is the difference between apparent and absolute magnitude?

Absolute and apparent magnitude are methods to measure the brightness of a star.

  • Absltue magnitude is a measure of the total power emitted by the star. We compute it with the formal M = -2.5 · log10(L/L0), where L is the star's luminosity and L0 a reference luminosity.
  • Apparent magnitude is a measure of the brightness of a star as seen from Earth. We use the formula m = m - 5 + 5 · log10(D), where D is the distance between the star and Earth.

How do I calculate the luminosity?

We compute luminosity with the following formula:
L = σ · A · T4

  • σStefan-Boltzmann constant, equal to 5.670367 × 10-8 W/(m2 · K4);
  • ASurface area (for a sphere, A = 4π · R2); and
  • TSurface temperature (which for stars can be determined through spectral analysis).

What is the luminosity of Vega?

47.67 L☉. To find this result:

  1. Find the radius of Vega and its surface temperature: R = 2.5 R☉ and T = 9,602 K.
  2. Find the surface temperature of the Sun and its luminosity: T☉ = 5,778 K and L☉ = 3.828 × 1026 W.
  3. Compute the ratios R/R☉ = 2.5 and T/T☉ = 9,602/5,778 = 1.66.
  4. Raise the first ratio to the power of two, the second to the power of 4, and multiply them: (R/R☉)2 · (T/T☉)4 = 2.52 · 1.664 = 47.67 L☉.

The result is Vega's luminosity in terms of Solar luminosity.

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