<p>When looking up the issue, I found surprisingly few publication that deal with such low mass stars and provide figures for their lifespan.
Namely, I have found only two:</p>
<p><a href="https://iopscience.iop.org/article/10.1086/304125" rel="nofollow noreferrer">The End of the Main Sequence: (1997) Laughlin, Bodenheimer, Adams</a></p>
<p>It deals with stars up to <span class="math-container">$0.25M_\odot$</span>, so only the convective ones. Figure 2 contains a small subfigure with the values of the lifespan of such stars. The plot is small and difficult to read, but fortunately Wikipedia provides a larger plot from the same data in the <a href="https://en.wikipedia.org/wiki/Red_dwarf#/media/File:Red_dwarf_lifetime.png" rel="nofollow noreferrer">Red Dwarf</a> page.</p>
<p><a href="https://ui.adsabs.harvard.edu/abs/1994A%26AS..105...29F/abstract" rel="nofollow noreferrer">Evolutionary sequences of stellar models with new radiative opacities. IV. Z=0.004 and Z=0.008: (1994) Fagotto, Bressan, Bertelli, Chiosi</a></p>
<p>Contains values for the duration of the main sequence and the core He burning for stars with <span class="math-container">$M&gt;0.6M_\odot$</span>. It gives them for two different metallicities (Z=0.004 and Z=0.008)</p>
<p>I wrote down the values of the lifespan of the stars provided in the two papers and made the following plot.</p>
<p><a href="https://i.sstatic.net/fDtF3.png" rel="nofollow noreferrer"><img src="https://i.sstatic.net/fDtF3.png" alt="enter image description here" /></a></p>
<p>I have fitted the points with power laws, and it appears indeed that there is some kind of transition between the two regimes. But it could also be due to different parameters and methods used in the two papers. Therefore I am not able to give a definitive answer to the question.</p>

CC BY-SA 4.0
2021-09-03T14:33:19.153Z
Interestingly, the lines seem to intersect at about 0.35 solar masses, which [the Wiki article on red dwarfs](https://en.wikipedia.org/wiki/Red_dwarf) says is the mass below which stars are fully convective.
zucculent
CC BY-SA 4.0
2021-09-03T11:33:53.377Z
2021-09-03T11:33:53.377Z
Prallax
<p>As already noted <a href="https://astronomy.stackexchange.com/a/46603">in another answer</a>, there aren't many studies about the long-term evolution of low-mass stars because we're fairly sure they don't evolve off the main sequence within the life of the Universe. But the answer inspired me to (quickly and roughly) compute the main-sequence lifetimes of some (roughly) solar metallicity objects between 0.15 and 0.80 solar masses using a <a href="https://docs.mesastar.org/" rel="noreferrer">stellar evolution program</a>. The models are fairly basic and I haven't the time to fully interpret them but they bear out the inference from the other answer.  I refined my parameter space around the transition at about 0.39 solar masses. The lifetimes do appear to decrease more rapidly as the mass approaches the transition from below.</p>
<p><a href="https://i.sstatic.net/TvXY1.png" rel="noreferrer"><img src="https://i.sstatic.net/TvXY1.png" alt="Double-logarithmic plot of approximate main-sequence lifetime versus stellar mass for between ~0.15 and 0.80 solar masses." /></a></p>

CC BY-SA 4.0
2021-09-08T12:38:00.940Z
Great answer! It must have really taken you a long time to run all these simulations with MESA! It also looks like your results are similar to what I have found in the literature
Prallax
CC BY-SA 4.0
2021-09-08T13:06:50.893Z
Not at all! Main sequence evolution is usually quite fast, especially at this quite coarse resolution and low mass. Even for quite detailed simulations, each evolution only takes a few minutes.
Warrick
CC BY-SA 4.0
2021-09-08T11:59:07.383Z
2021-09-08T11:59:07.383Z
Warrick
<p>A star with less than a certain mass <em>M</em>, which is somewhere between 0.5 and 0.35 solar masses, is fully convective, the hydrogen in the core is constantly being replenished, so it takes much longer for the star to run out of fuel. A star with more than mass <em>M</em> has a radiative center, meaning the core can no longer be replenished. Does this cause a sudden and drastic decrease in the star's lifespan?</p>

<star><stellar-structure>
Does the transition between total convection and partial convection cause a significant decrease in lifespan?
zucculent
# Does the transition between total convection and partial convection cause a significant decrease in lifespan?

(Asked by: username_0 on 2021-09-02)

A star with less than a certain mass *M*, which is somewhere between 0.5 and 0.35 solar masses, is fully convective, the hydrogen in the core is constantly being replenished, so it takes much longer for the star to run out of fuel. A star with more than mass *M* has a radiative center, meaning the core can no longer be replenished. Does this cause a sudden and drastic decrease in the star's lifespan?

**Tags:** star, stellar-structure


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## 2 answers

### Answer by username_2 on 2021-09-08. Score: 5 | Accepted answer

As already noted [in another answer](https://astronomy.stackexchange.com/a/46603), there aren't many studies about the long-term evolution of low-mass stars because we're fairly sure they don't evolve off the main sequence within the life of the Universe. But the answer inspired me to (quickly and roughly) compute the main-sequence lifetimes of some (roughly) solar metallicity objects between 0.15 and 0.80 solar masses using a [stellar evolution program](https://docs.mesastar.org/). The models are fairly basic and I haven't the time to fully interpret them but they bear out the inference from the other answer. I refined my parameter space around the transition at about 0.39 solar masses. The lifetimes do appear to decrease more rapidly as the mass approaches the transition from below.

[![Double-logarithmic plot of approximate main-sequence lifetime versus stellar mass for between ~0.15 and 0.80 solar masses.](https://i.sstatic.net/TvXY1.png)](https://i.sstatic.net/TvXY1.png)

> **Comments:**
> **username_1**: Great answer! It must have really taken you a long time to run all these simulations with MESA! It also looks like your results are similar to what I have found in the literature  
> **username_2**: Not at all! Main sequence evolution is usually quite fast, especially at this quite coarse resolution and low mass. Even for quite detailed simulations, each evolution only takes a few minutes.  

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### Answer by username_1 on 2021-09-03. Score: 3

When looking up the issue, I found surprisingly few publication that deal with such low mass stars and provide figures for their lifespan.
Namely, I have found only two:

[The End of the Main Sequence: (1997) Laughlin, Bodenheimer, Adams](https://iopscience.iop.org/article/10.1086/304125)

It deals with stars up to $0.25M\_\odot$, so only the convective ones. Figure 2 contains a small subfigure with the values of the lifespan of such stars. The plot is small and difficult to read, but fortunately Wikipedia provides a larger plot from the same data in the [Red Dwarf](https://en.wikipedia.org/wiki/Red_dwarf#/media/File:Red_dwarf_lifetime.png) page.

[Evolutionary sequences of stellar models with new radiative opacities. IV. Z=0.004 and Z=0.008: (1994) Fagotto, Bressan, Bertelli, Chiosi](https://ui.adsabs.harvard.edu/abs/1994A%26AS..105...29F/abstract)

Contains values for the duration of the main sequence and the core He burning for stars with $M>0.6M\_\odot$. It gives them for two different metallicities (Z=0.004 and Z=0.008)

I wrote down the values of the lifespan of the stars provided in the two papers and made the following plot.

[![enter image description here](https://i.sstatic.net/fDtF3.png)](https://i.sstatic.net/fDtF3.png)

I have fitted the points with power laws, and it appears indeed that there is some kind of transition between the two regimes. But it could also be due to different parameters and methods used in the two papers. Therefore I am not able to give a definitive answer to the question.

> **Comments:**
> **username_0**: Interestingly, the lines seem to intersect at about 0.35 solar masses, which [the Wiki article on red dwarfs](https://en.wikipedia.org/wiki/Red_dwarf) says is the mass below which stars are fully convective.  

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