<p>The difference between a brown dwarf and a star is not a sharp boundary. A brown dwarf is simply a ball of gas where the (small) fusion rate is incapable of providing a significant fraction of the luminosity (which is mainly provided by gravitational contraction).</p>

<p>A star will contract and reach a minimum luminosity, whilst a brown dwarf's luminosity will monotonically decrease throughout its life. The core becomes degenerate and it is this that provides the pressure that supports a brown dwarf, even though it becomes colder.</p>

<p>If you add some mass to a brown dwarf, then the result depends when you add it. If you add it early during the strong contraction phase then you might get a low-mass star. If it is added after the brown dwarf is degenerate, then it could contract further, but do so without increasing the temperature enough to ignite hydrogen strongly. This is an interesting problem that deserves a model simulation!</p>

<p>If fusion can start to any degree, then convective mixing in these very low mass objects will very gradually (<em>trillions</em> of years), turn nearly all their H to He.</p>

CC BY-SA 3.0
2016-05-12T13:20:20.310Z
2016-05-12T13:56:39.847Z
2016-05-12T13:56:39.847Z
ProfRob
<p>Suppose a brown dwarf requires only one more hydrogen atom to become massive enough to start fusion, what will happen if we add a hydrogen atom to it?</p>

<ol>
<li><p>It fuses until the mass is dropped and then fusion stops suddenly</p></li>
<li><p>It starts to fuse until all hydrogen use up</p></li>
</ol>

<p>Which one is correct?</p>

CC BY-SA 3.0
2016-05-12T10:45:29.107Z
It's an interesting question what happens at that border between M9V Red Dwarfs and the heaviest Brown dwarfs.  Have you read about lighter red dwarfs, below .35 solar masses they undergo convection which enables them to fuse a higher percentage of hydrogen, then as they slowly cool they condense, which makes them hotter (cooling makes them hotter, I know), eventually becoming white dwarfs.   The mass and perhaps metalicity boundary between a white dwarf future vs a permanent Brown dwarf is an interesting question.   https://en.wikipedia.org/wiki/Red_dwarf#Description_and_characteristics
userLTK
CC BY-SA 3.0
2016-05-12T13:25:28.193Z
I'd expect there's a mass range there where you get periodic, oscillatory, fusion reactions in the near-star.
Wayfaring Stranger
<star>
Do stars tend to fuse all hydrogen even when the mass is small?
Gstestso
# Do stars tend to fuse all hydrogen even when the mass is small?

(Asked by: username_0 on 2016-05-12)

Suppose a brown dwarf requires only one more hydrogen atom to become massive enough to start fusion, what will happen if we add a hydrogen atom to it?

1. It fuses until the mass is dropped and then fusion stops suddenly
2. It starts to fuse until all hydrogen use up

Which one is correct?

**Tags:** star

> **Comments:**
> **username_1**: It's an interesting question what happens at that border between M9V Red Dwarfs and the heaviest Brown dwarfs.  Have you read about lighter red dwarfs, below .35 solar masses they undergo convection which enables them to fuse a higher percentage of hydrogen, then as they slowly cool they condense, which makes them hotter (cooling makes them hotter, I know), eventually becoming white dwarfs.   The mass and perhaps metalicity boundary between a white dwarf future vs a permanent Brown dwarf is an interesting question.   https://en.wikipedia.org/wiki/Red_dwarf#Description_and_characteristics  
> **username_2**: I'd expect there's a mass range there where you get periodic, oscillatory, fusion reactions in the near-star.  

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## 1 answers

### Answer by username_3 on 2016-05-12. Score: 7 | Accepted answer

The difference between a brown dwarf and a star is not a sharp boundary. A brown dwarf is simply a ball of gas where the (small) fusion rate is incapable of providing a significant fraction of the luminosity (which is mainly provided by gravitational contraction).

A star will contract and reach a minimum luminosity, whilst a brown dwarf's luminosity will monotonically decrease throughout its life. The core becomes degenerate and it is this that provides the pressure that supports a brown dwarf, even though it becomes colder.

If you add some mass to a brown dwarf, then the result depends when you add it. If you add it early during the strong contraction phase then you might get a low-mass star. If it is added after the brown dwarf is degenerate, then it could contract further, but do so without increasing the temperature enough to ignite hydrogen strongly. This is an interesting problem that deserves a model simulation!

If fusion can start to any degree, then convective mixing in these very low mass objects will very gradually (*trillions* of years), turn nearly all their H to He.


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