<p>The luminosity of a star remains approximately constant during its time on the main sequence. There is a slight increase over time, which is, as you guessed, related to the changing composition of the star due to fusion.</p>

<p>The so-called <a href="https://en.wikipedia.org/wiki/Vogt%E2%80%93Russell_theorem" rel="nofollow noreferrer">Vogt-Russell theorem</a> tells us that a star's mass and composition are the only two factors that affect its structure and, by extension, its luminosity.<span class="math-container">$^{\dagger}$</span> Most main sequence stars have negligible mass-loss rates (at least, compared to evolved stars like AGB stars), and so therefore compositional changes should be the only thing dictating luminosity evolution.</p>

<p>It turns out that <a href="https://www.astro.ru.nl/~onnop/education/stev_utrecht_notes/chapter9-11.pdf" rel="nofollow noreferrer">the luminosity is related to the mean molecular mass <span class="math-container">$\mu$</span></a> by (approximately)
<span class="math-container">$$L\propto\mu^4$$</span>
which is not insignificant. Fusion turns hydrogen to helium in the star's core, and hence there should be an increase in <span class="math-container">$\mu$</span> and thus in luminosity (roughly a factor of two). The change is small compared to the orders of magnitude by which two main sequence stars may differ from one another, but it isn't zero.</p>

<p>As an aside, there is indeed a change in the central temperature (though I would note that your use of the Stefan-Boltzmann law requires a change in the <em>surface temperature</em>) to accommodate the increase in luminosity, but the energy generation rate is very sensitive to changes in temperature, particularly for stars using the CNO cycle.</p>

<hr>

<p><span class="math-container">$^{\dagger}$</span> This is, strictly speaking, not true. Rotation, as Rob Jeffries mentioned, is also important for certain stars, and it can have a role on the evolution of a star's luminosity.</p>

CC BY-SA 4.0
2020-05-07T22:13:42.163Z
Still, the small increase in the Sun's luminosity will start to disrupt the Earth's carbonate-silicate cycle in about 500 million years, and by 1.2 billion years the mean surface temperature will be 47°C and the Earth will be virtually uninhabitable. See https://en.wikipedia.org/wiki/Timeline_of_the_far_future#Future_of_the_Earth,_the_Solar_System_and_the_universe
PM 2Ring
CC BY-SA 4.0
2020-05-07T23:57:45.927Z
@PM2Ring From a human (or planetary?) point of view, yes, the changes are certainly significant.
HDE 226868
CC BY-SA 4.0
2020-05-08T07:17:19.510Z
It depends on what you consider 'constant'. While on main sequence, the luminosity doesn't change orders of magnitude, a change of several 10% over the life of the star on main sequence is possible (sun got brighter by about 20% in the last 4.5 billion years)
planetmaker
CC BY-SA 4.0
2020-05-08T12:04:34.990Z
The change is more like a factor of two over the main sequence lifetime.
ProfRob
CC BY-SA 4.0
2020-05-08T12:06:47.757Z
The Vogt-Russell theorem also ignores rotation. This turns out to influence the rate of change of luminosity greatly (in stars more massive than the Sun).
ProfRob
CC BY-SA 4.0
2020-05-08T20:28:00.887Z
@RobJeffries Thank you; that's quite a good point.
HDE 226868
CC BY-SA 4.0
2020-05-07T21:43:35.333Z
2020-05-08T20:36:56.190Z
2020-05-08T20:36:56.190Z
HDE 226868
<p>From my understanding, the luminosity of a main sequence star should increase because, in its core, hydrogen is being burnt into helium which means that the number density of hydrogen decreases and the temperature increases and from the Stefan–Boltzmann law, the temperature is proportional to the luminosity so the luminosity of a star should increase while it's on the main sequence phase of evolution. </p>

<p>Please correct me if my reasoning is incorrect.</p>

<luminosity><stellar-astrophysics><core><main-sequence>
Does the luminosity of a star on its main sequence increase or remain approximately constant?
MAXX
# Does the luminosity of a star on its main sequence increase or remain approximately constant?

(Asked by: username_0 on 2020-05-07)

From my understanding, the luminosity of a main sequence star should increase because, in its core, hydrogen is being burnt into helium which means that the number density of hydrogen decreases and the temperature increases and from the Stefan–Boltzmann law, the temperature is proportional to the luminosity so the luminosity of a star should increase while it's on the main sequence phase of evolution.

Please correct me if my reasoning is incorrect.

**Tags:** luminosity, stellar-astrophysics, core, main-sequence

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## 1 answers

### Answer by username_1 on 2020-05-07. Score: 4

The luminosity of a star remains approximately constant during its time on the main sequence. There is a slight increase over time, which is, as you guessed, related to the changing composition of the star due to fusion.

The so-called [Vogt-Russell theorem](https://en.wikipedia.org/wiki/Vogt%E2%80%93Russell_theorem) tells us that a star's mass and composition are the only two factors that affect its structure and, by extension, its luminosity.$^{\dagger}$ Most main sequence stars have negligible mass-loss rates (at least, compared to evolved stars like AGB stars), and so therefore compositional changes should be the only thing dictating luminosity evolution.

It turns out that [the luminosity is related to the mean molecular mass $\mu$](https://www.astro.ru.nl/~onnop/education/stev_utrecht_notes/chapter9-11.pdf) by (approximately)
$$L\propto\mu^4$$
which is not insignificant. Fusion turns hydrogen to helium in the star's core, and hence there should be an increase in $\mu$ and thus in luminosity (roughly a factor of two). The change is small compared to the orders of magnitude by which two main sequence stars may differ from one another, but it isn't zero.

As an aside, there is indeed a change in the central temperature (though I would note that your use of the Stefan-Boltzmann law requires a change in the *surface temperature*) to accommodate the increase in luminosity, but the energy generation rate is very sensitive to changes in temperature, particularly for stars using the CNO cycle.

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$^{\dagger}$ This is, strictly speaking, not true. Rotation, as Rob Jeffries mentioned, is also important for certain stars, and it can have a role on the evolution of a star's luminosity.

> **Comments:**
> **username_2**: Still, the small increase in the Sun's luminosity will start to disrupt the Earth's carbonate-silicate cycle in about 500 million years, and by 1.2 billion years the mean surface temperature will be 47°C and the Earth will be virtually uninhabitable. See https://en.wikipedia.org/wiki/Timeline_of_the_far_future#Future_of_the_Earth,_the_Solar_System_and_the_universe  
> **username_1**: @PM2Ring From a human (or planetary?) point of view, yes, the changes are certainly significant.  
> **username_3**: It depends on what you consider 'constant'. While on main sequence, the luminosity doesn't change orders of magnitude, a change of several 10% over the life of the star on main sequence is possible (sun got brighter by about 20% in the last 4.5 billion years)  
> **username_4**: The change is more like a factor of two over the main sequence lifetime.  
> **username_4**: The Vogt-Russell theorem also ignores rotation. This turns out to influence the rate of change of luminosity greatly (in stars more massive than the Sun).  
> **username_1**: @RobJeffries Thank you; that's quite a good point.  

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