<p>I don't have detailed model calculations to hand and I'm not sure they have been done for the small range of metallicity you mention. However, in handwaving terms.</p>

<p>(1) Mass and composition are the most important variables. Helium abundance, in addition to metallicity, could play a role. Rotation could be a very second order effect. Very rapid rotation would lower core temperatures at the same mass.</p>

<p>(2) This is the general assumption if a star plus brown dwarf companion formed in a binary or even if they formed in the same cluster.</p>

<p>(3) Higher metallicity leads to larger opacity in the atmosphere and a larger brown dwarf. This is a small effect in fully convective objects like these, except perhaps when they are very young and have superadiabatic surface layer. However, as this is when D burning takes place, possibly there is a small effect - higher metallicity leads to a larger radius for the same mass and a lower core temperature. So the mass threshold would be slightly higher.</p>

<p>(4) The duration of D burning is mass dependent. The graph below, from <a href="https://arxiv.org/abs/astro-ph/9705201" rel="nofollow noreferrer">Burrows et al. (1997)</a>, shows luminosity vs time for brown dwarfs, planets and stars. The D burning phase is the early plateau in luminosity, lasting a few million years for things which are almost stars to maybe one or two hundred million years at 13 Jupiter masses. When D fusion ceases, then cooling recommences and the luminosity will continue to fade (forever), unless the object is massive enough to ignite hydrogen (i.e. a star: the difference between the green lines and blue lines on the plot).</p>

<p><a href="https://i.sstatic.net/OoRsc.png" rel="nofollow noreferrer"><img src="https://i.sstatic.net/OoRsc.png" alt="Burrows 97 calculations"></a></p>

CC BY-SA 3.0
2017-08-29T03:31:18.710Z
The overlapping on the graph above is interesting. It appears that, in this model, there is an "era" between about 40 million years to 400 million years that a 0.015 M(sun) brown dwarf outshines a 0.02 M(sun) brown dwarf.
Jack R. Woods
CC BY-SA 3.0
2017-08-28T20:28:36.093Z
2017-08-29T07:04:49.257Z
2017-08-29T07:04:49.257Z
ProfRob
<p>I've read that when a body reaches about 13 times the mass of Jupiter that deuterium fusion starts and the body becomes a brown dwarf instead of a planet.</p>

<p>I have a multiple question.</p>

<ul>
<li><p>Are there any other factors besides mass and possibly metal abundance (composition) that would determine this "turn on" point ?</p></li>
<li><p>If the "brown dwarf" was detected indirectly and no spectroscopic information was available, could we assume that metalicity would be the same as the larger star ?</p></li>
<li><p>Would a higher metallicity body "turn on" at a lower mass? (Would a difference between [Fe/H] = -0.19 and [Fe/H] = +0.07 make much of a difference in "turn on mass"?)</p></li>
</ul>

<p>*I did miss the related question when I posted this one, but I do have a question here that wasn't answered. It was about how stellar metallicity effects the onset of fusion. I think it may be as simple as whether or not adding "metals" makes the core hotter or colder for a given mass. I also wanted to know if I could assume that both "stars" in a binary system should have the same metallicity.</p>

<p>*Now that I've read Rob's excellent (as usual) answer, I would be curious as to how long deuterium fusion lasts in brown dwarfs from 13 to 80 Jupiter masses and what happens (in models) when it stops.</p>

CC BY-SA 3.0
2017-08-28T10:18:25.843Z
Related, if not a duplicate: https://astronomy.stackexchange.com/questions/10331/what-is-the-minimum-size-of-a-ball-of-gas-to-become-a-star
David Hammen
CC BY-SA 3.0
2017-08-28T12:36:55.637Z
Possible duplicate of [What is the minimum size of a ball of gas to become a star?](https://astronomy.stackexchange.com/questions/10331/what-is-the-minimum-size-of-a-ball-of-gas-to-become-a-star)
Carl Witthoft
CC BY-SA 3.0
2017-08-28T20:05:54.390Z
The proposed duplicate is about stars?? This is asking about deuterium fusion in brown dwarfs (I think).
ProfRob
CC BY-SA 3.0
2017-08-28T20:07:37.817Z
The 13 Jupiter mass threshold is that for D burning, not the threshold of starhood, which is at around 70 Jupiter masses.
ProfRob
<brown-dwarf><nucleosynthesis>
"Turn on point" for fusion?
Jack R. Woods
# "Turn on point" for fusion?

(Asked by: username_0 on 2017-08-27)

I've read that when a body reaches about 13 times the mass of Jupiter that deuterium fusion starts and the body becomes a brown dwarf instead of a planet.

I have a multiple question.

* Are there any other factors besides mass and possibly metal abundance (composition) that would determine this "turn on" point ?
* If the "brown dwarf" was detected indirectly and no spectroscopic information was available, could we assume that metalicity would be the same as the larger star ?
* Would a higher metallicity body "turn on" at a lower mass? (Would a difference between [Fe/H] = -0.19 and [Fe/H] = +0.07 make much of a difference in "turn on mass"?)

\*I did miss the related question when I posted this one, but I do have a question here that wasn't answered. It was about how stellar metallicity effects the onset of fusion. I think it may be as simple as whether or not adding "metals" makes the core hotter or colder for a given mass. I also wanted to know if I could assume that both "stars" in a binary system should have the same metallicity.

\*Now that I've read Rob's excellent (as usual) answer, I would be curious as to how long deuterium fusion lasts in brown dwarfs from 13 to 80 Jupiter masses and what happens (in models) when it stops.

**Tags:** brown-dwarf, nucleosynthesis

> **Comments:**
> **username_1**: Related, if not a duplicate: https://astronomy.stackexchange.com/questions/10331/what-is-the-minimum-size-of-a-ball-of-gas-to-become-a-star  
> **username_2**: Possible duplicate of [What is the minimum size of a ball of gas to become a star?](https://astronomy.stackexchange.com/questions/10331/what-is-the-minimum-size-of-a-ball-of-gas-to-become-a-star)  
> **username_3**: The proposed duplicate is about stars?? This is asking about deuterium fusion in brown dwarfs (I think).  
> **username_3**: The 13 Jupiter mass threshold is that for D burning, not the threshold of starhood, which is at around 70 Jupiter masses.  

---

## 1 answers

### Answer by username_3 on 2017-08-28. Score: 5 | Accepted answer

I don't have detailed model calculations to hand and I'm not sure they have been done for the small range of metallicity you mention. However, in handwaving terms.

(1) Mass and composition are the most important variables. Helium abundance, in addition to metallicity, could play a role. Rotation could be a very second order effect. Very rapid rotation would lower core temperatures at the same mass.

(2) This is the general assumption if a star plus brown dwarf companion formed in a binary or even if they formed in the same cluster.

(3) Higher metallicity leads to larger opacity in the atmosphere and a larger brown dwarf. This is a small effect in fully convective objects like these, except perhaps when they are very young and have superadiabatic surface layer. However, as this is when D burning takes place, possibly there is a small effect - higher metallicity leads to a larger radius for the same mass and a lower core temperature. So the mass threshold would be slightly higher.

(4) The duration of D burning is mass dependent. The graph below, from [Burrows et al. (1997)](https://arxiv.org/abs/astro-ph/9705201), shows luminosity vs time for brown dwarfs, planets and stars. The D burning phase is the early plateau in luminosity, lasting a few million years for things which are almost stars to maybe one or two hundred million years at 13 Jupiter masses. When D fusion ceases, then cooling recommences and the luminosity will continue to fade (forever), unless the object is massive enough to ignite hydrogen (i.e. a star: the difference between the green lines and blue lines on the plot).

[![Burrows 97 calculations](https://i.sstatic.net/OoRsc.png)](https://i.sstatic.net/OoRsc.png)

> **Comments:**
> **username_0**: The overlapping on the graph above is interesting. It appears that, in this model, there is an "era" between about 40 million years to 400 million years that a 0.015 M(sun) brown dwarf outshines a 0.02 M(sun) brown dwarf.  

---

