The Mass Luminosity Relationship applies only to main sequence stars  those stars which produce energy by fusing hydrogen into helium.
The amount of mass in a main sequence star affects many of its properties.
Generally speaking, if we are comparing 2 stars, the star with the greater mass will have:
• Higher Luminosity (and brighter absolute magnitude)
• Larger Radius
• Hotter Temperature
• A shorter lifetime and a more violent "death"
• A bluer color, and a "bluer" spectral type
Let's first discuss how mass affects luminosity.
Effect of Star Mass On Luminosity
There is an equation that relates star mass and luminosity.
That equation is not an exact rule but it provides a good approximation.
Where luminosity and mass are based on the Sun = 1.
So, if a star is 3 times more massive than the Sun, it will have a luminosity that is 46.8 times brighter.
3^{3.5} = 46.8
Since we have calculated the luminosity, we can calculate the absolute magnitude with this formula:
Absolute Magnitude = 4.83 ⚊2.5 • log_{10}(46.8)
Absolute Magnitude = 4.83 ⚊2.5 • 1.6702458531
Absolute Magnitude = 4.83 ⚊4.1756146328
Absolute Magnitude = 0.6543853673
Effect of Star Mass On Radius
It makes sense that if a star has more mass, it will have a bigger radius.
In fact, here are the equations for calculating a star's radius based on its mass.
Where radius and mass are based on the Sun = 1.
So, a star with half the mass of the Sun will have a radius of .5^{.80} = .574
and a star with twice the mass of the Sun will have a radius of 2^{.57} = 1.48.
Effect of Star Mass On Temperature
The star with the higher mass will have a higher surface temperature.
You have probably seen the following equation in many web pages and books:
Temperature ∝ (Luminosity / radius²)^{¼}
However, that formula is not very accurate at all.
A more appropriate equation is:
Although that equation is very accurate, we can further simplify it:
Let's use the above equation to calculate the surface temperature of the Sun:
Sun's Luminosity = 3.828 x 10³³ ergs.
Sun's Surface Area = 6.09421 x 10²² square centimeters.
Temperature = 3.828 x 10³³ ergs ÷ (6.09421 x 10²² cm² • .000056704 erg/cm²•K⁴)^{¼}
Temperature = 3.828 x 10³³ ÷ (3.46 x 10¹⁸ K⁴)^{¼}
Temperature = (1.11 x 10¹⁵ K⁴)^{¼}
Temperature = 5,769 Kelvin
Effect of Star Mass On Longevity
It would seem common sense that if a star had higher mass, it should live longer but this is not the case.
The more massive a star becomes, its greater gravity requires higher temperatures and pressures to prevent gravitational collapse. The energy required for this causes the star to use up fuel at a rather furious rate.
So, a star that has 10 times the mass of the Sun has 10 times the fuel. However, as we know from the mass luminosity formula, the star will be consuming fuel at a rate equal to its mass to the 3.5 power.
Combining these two factors, a star's mass will decrease (or increase) its lifetime by a factor of [mass] ^{2.5}.
Knowing that the Sun will have a lifetime of 10 billion years, we can come up with this formula:
Using that formula, we calculated the following data (where "mass" is the Sun's mass equal to one) and the "years" is the predicted lifetime of the star.
Mass  Years 
Mass  Years 
Mass  Years 
Mass  Years 
0.080  5,500,000,000,000 
0.50  57,000,000,000 
2.50  1,000,000,000 
20.00  5,600,000 
0.100  3,200,000,000,000 
0.75  21,000,000,000 
3.00  640,000,000 
25.00  3,200,000 
0.125  1,800,000,000,000 
1.00  10,000,000,000 
4.00  310,000,000 
40.00  990,000 
0.150  1,100,000,000,000 
1.25  5,700,000,000 
5.00  180,000,000 
50.00  570,000 
0.200  560,000,000,000 
1.50  3,600,000,000 
10.00  32,000,000 
100.00  100,000 
0.250  320,000,000,000 
2.00  1,800,000,000 
12.50  18,000,000 
150.00  36,000 
A more massive star has a shorter lifetime and a more violent death than a lower mass star.
The lowest possible mass of a star is about .08 the mass of the Sun.
Depending on the star's mass, we have made a table showing how each type of star ages.
Mass  Evolves Into ****************************************************************** 
0.08 to .50  After Hydrogen to Helium fusion ends, it becomes a white dwarf. 
> 0.50 and < 1.5  Hydrogen to Helium fusion ends then star gets larger, becoming a red giant, eventually forming a planetary nebula, then becomes a white dwarf. 
1.5 and < 3.2  Becomes a red supergiant then becomes a supernova and finally forms a neutron star. 
>= 3.2  Becomes a red supergiant then becomes a supernova and finally forms a black hole. 
Effect of Star Mass On Spectral Type and Color
This can easily be presented as a table.
Mass  Spectral Type  Color 
>=16  O  blue 
2.10 to 16  B  blue white 
1.40 to 2.10  A  white 
1.04 to 1.40  F  yellow white 
.80 to 1.04  G  yellow 
.45 to .80  K  orange 
.08 to .45  M  red 
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