<p>This is an important question to ask about the <a href="https://en.wikipedia.org/wiki/Initial_mass_function" rel="noreferrer">initial mass functio</a>n of objects in the Galaxy - and the final answer hasn't been cast as it is a matter of research.</p>
<p>Yet, observational data (e.g. see the mass functions for various clusters in <a href="https://astro.uni-bonn.de/%7Epavel/HLmeeting/2006/talks/thies.pdf" rel="noreferrer">this talk</a>), and simulations in more or less good agreement with that (e.g. <a href="https://arxiv.org/pdf/1205.2966.pdf" rel="noreferrer">here</a> or <a href="https://arxiv.org/pdf/1501.01640.pdf" rel="noreferrer">here</a>), seem to indicate that this so-called <a href="https://en.wikipedia.org/wiki/Brown-dwarf_desert" rel="noreferrer">brown dwarf desert</a> is real and that we talk about fundamentally different formation mechanisms between stars and planets. Yet this doesn't mean that no such objects exist nor do we completely understand the causes for these observational findings. One thing playing a role here could be that there is a lower limit to the <a href="https://arxiv.org/pdf/2008.06396.pdf" rel="noreferrer">Jeans mass</a> (or rather density) which you will not pass for a single star / brown dwarf by fluctuations in a collapsing gas cloud due to thermodynamics - which seems to be around the Brown dwarf mass.</p>
<p>Just recently there have been attempts to get a better handle on some Brown Dwarfs by help of transit detection (e.g. see <a href="https://www.aanda.org/articles/aa/full_html/2019/08/aa35505-19/aa35505-19.html" rel="noreferrer">here</a>) which allows to constrain its parameter much better than before.</p>

CC BY-SA 4.0
2021-07-01T10:56:55.583Z
And I wonder whether reference 3 is written by a certain member of this SE and whether he could thus write a much better answer :)
planetmaker
CC BY-SA 4.0
2021-07-01T10:55:32.260Z
2021-07-01T10:55:32.260Z
planetmaker
<p>According to the <a href="https://en.wikipedia.org/wiki/Sub-brown_dwarf" rel="nofollow noreferrer">wiki</a> article on sub-brown dwarfs, the lowest mass object that can form from collapse of gas cloud is about 1 Jupiter mass.</p>
<p>Original source: <a href="https://ui.adsabs.harvard.edu/abs/2003IAUS..211..529B/abstract" rel="nofollow noreferrer">Boss, Alan P.; Basri, Gibor; Kumar, Shiv S.; Liebert, James; Martín, Eduardo L.; Reipurth, Bo; Zinnecker, Hans (2003), &quot;Nomenclature: Brown Dwarfs, Gas Giant Planets, and ?&quot;</a></p>

CC BY-SA 4.0
2021-07-01T17:39:36.073Z
How can that be, when Neptune, Uranus and Saturn are also gas giants?
RonJohn
CC BY-SA 4.0
2021-07-01T18:47:45.367Z
Those are planets. They likely formed by accretion in a protoplanetary disk around the sun, not from collapse of gas cloud.
sno
CC BY-SA 4.0
2021-07-02T06:59:35.700Z
@RonJohn if it hasn't been asked already, that might make a good new question.
uhoh
CC BY-SA 4.0
2021-07-02T16:31:33.543Z
Please cite original work, not wikipedia where possible. It clearly is possible in this case.
ProfRob
CC BY-SA 4.0
2021-07-01T12:35:50.317Z
2021-07-31T16:46:14.400Z
2021-07-31T16:46:14.400Z
sno
<p>The answer to your first question is (now) fairly simple: No, brown dwarfs are <em>not</em> more common than red dwarfs. A crude approximation is that stars (which are indeed mostly red dwarfs) outnumber brown dwarfs 4 or 5 to 1; see, for example, the review article by <a href="https://arxiv.org/abs/1401.7559" rel="nofollow noreferrer">Chabrier et al. (2014)</a>. This is supported by extensive surveys done in the 2000s and 2010s, including observations with the WISE telescope; these are sensitive enough to uncover quite faint brown dwarfs.</p>
<p>Empirically, attempts to count stars and brown dwarfs in local volumes strongly suggest that stars outnumber brown dwarfs. For example, <a href="https://arxiv.org/abs/2104.14972" rel="nofollow noreferrer">Reylé et al. (2021)</a> combine <em>Gaia</em> observations (sensitive to hydrogen-burning stars and the more massive brown dwarfs) with literature observations of brown dwarfs using IR telescopes (<em>Spitzer</em>, <em>WISE</em>) to make a census of different objects within 10 pc (33 light years) of the Sun. They find a total of 355 (hydrogen-burning) stars -- including 276 M dwarfs --, 20 white dwarfs (formerly hydrogen-burning), and 85 brown dwarfs (plus 3 more candidates). They do note that there are probably more brown dwarfs waiting to be identified, though these would have to be at the very low-mass (and thus low-luminosity) end. One can still argue that stars outnumber brown dwarfs in our local volume by about three or four to one.</p>
<p>It is true that lower mass stars tend to be more common than higher mass stars. However, this trend becomes weaker for lower masses. The figure below (from the Wikipedia article on the <a href="https://en.wikipedia.org/wiki/Initial_mass_function" rel="nofollow noreferrer">initial mass function (IMF) of stars</a>, which tells you how many stars of a given mass are born, as a function of mass) shows several different versions of the IMF. The best current measurements are encoded in either the &quot;Kroupa01&quot; or &quot;Chabrier03&quot; curves, all of which show that the curves flatten -- or even turn over -- for very low masses. This means that if you add up all the brown dwarfs and add up all the stars, you end up with more stars than brown dwarfs.</p>
<p><strong>Edited to add:</strong> Empirical counts of stars and brown dwarfs in the local volume.</p>
<p><a href="https://i.sstatic.net/Psio1.png" rel="nofollow noreferrer"><img src="https://i.sstatic.net/Psio1.png" alt="enter image description here" /></a></p>

CC BY-SA 4.0
2021-07-02T19:22:48.453Z
Your first citation that red dwarfs outnumber brown 4-to-1 uses an IMF not shown in your plot. The Chabrier 03 you show has the peak mass at 8% solar, whereas the 4-to-1 calculation uses 25% solar. Using 8% solar flips things so brown outnumber red 4-to-1. The ratio appears to be highly uncertain.
Xerxes
CC BY-SA 4.0
2021-07-03T16:58:52.377Z
@Xerxes I'm not sure how you're getting 4-to-1 brown-dwarfs to M dwarfs for the Chabrier03 IMF; my integration suggests 1-to-1.4. In any case, I've updated my answer with some notes on observed local counts, which tends to agree with the 4-to-1 stars-to-brown-dwarfs estimate.
Peter Erwin
CC BY-SA 4.0
2021-07-31T17:15:41.877Z
There are *observations* in open clusters (rather than proposed mass functions) which support the 4 stars to 1 BD figure.
ProfRob
CC BY-SA 4.0
2021-07-01T12:27:58.530Z
2021-07-03T16:27:07.360Z
2021-07-03T16:27:07.360Z
Peter Erwin
<p>I <a href="https://youtu.be/uZRDONE4zng?t=831" rel="noreferrer">recently heard</a> that Red Dwarfs are the most common type of star, and low-mass Red Dwarfs are the most common type of Red Dwarf.  This seems to imply a generic trend that the lower the mass, the more common the star.  I have 2 questions.</p>
<ol>
<li><p>I know that Brown Dwarfs and Sub-Brown Dwarfs are much harder to detect because they are not very luminous.  Is it possible that Brown Dwarfs and Sub-Brown Dwarfs are actually even more common than Red Dwarfs?  Are there any theories or papers on this?</p>
</li>
<li><p>Is there a lower limit on the mass of an object that can be formed at the center of a gas/dust nebula collapse (as opposed to being formed in a protoplanetary disk)?</p>
</li>
</ol>

CC BY-SA 4.0
2021-07-01T11:59:25.137Z
What do you mean by "Sub-Brown Dwarfs"?
Peter Erwin
CC BY-SA 4.0
2021-07-01T17:32:00.817Z
*Secretly* more common?
RonJohn
CC BY-SA 4.0
2021-07-01T21:04:55.723Z
Aren’t Sub-brown dwarfs called “planets”?
RBarryYoung
CC BY-SA 4.0
2021-07-02T02:35:39.993Z
Sub-brown dwarfs also known as planetary-mass brown dwarfs are formed like stars from collapse of a gas cloud, unlike planets which are formed by accretion in a protoplanetary disk. https://en.wikipedia.org/wiki/Sub-brown_dwarf
sno
CC BY-SA 4.0
2021-07-03T18:16:08.823Z
LISA gravitational wave observatory is expected to shed light on the brown dwarf desert/gap https://arxiv.org/abs/1903.02049 and https://arxiv.org/abs/1910.05414 for examples
Daddy Kropotkin
CC BY-SA 4.0
2021-07-06T21:15:12.290Z
@RBarryYoung, Sub-brown dwarfs are a subset of planets.  Only planets that are formed in the same manner as stars and brown dwarfs can be called sub-brown dwarfs.  Any planet formed in a protoplanetary disc cannot be called a sub-brown dwarf.
cowlinator
CC BY-SA 4.0
2023-09-22T05:43:40.953Z
The Starforge simulations helped provide me with some visual intuition about why brown dwarves might be less common (theoretically). In the simulations, proto-stars in a nebula continue to gravitationally attract more gas until fusion triggers outward stellar winds, which drives away all nearby free gas. This stops the growth of the star. Brown dwarves don't have stellar winds, so there is nothing to stop growth (unless they happen to run out of gas).  https://www.youtube.com/watch?v=qh9TCg-3zus&list=PLtrvxOPz9tAMrMMw7m1I1j4iaXUNB4BK5&index=1
cowlinator
<nebula><brown-dwarf><rogue-planet><red-dwarf><protostar>
Are Brown and Sub-Brown Dwarfs secretly more common than stars?
cowlinator
# Are Brown and Sub-Brown Dwarfs secretly more common than stars?

(Asked by: username_0 on 2021-07-01)

I [recently heard](https://youtu.be/uZRDONE4zng?t=831) that Red Dwarfs are the most common type of star, and low-mass Red Dwarfs are the most common type of Red Dwarf. This seems to imply a generic trend that the lower the mass, the more common the star. I have 2 questions.

1. I know that Brown Dwarfs and Sub-Brown Dwarfs are much harder to detect because they are not very luminous. Is it possible that Brown Dwarfs and Sub-Brown Dwarfs are actually even more common than Red Dwarfs? Are there any theories or papers on this?
2. Is there a lower limit on the mass of an object that can be formed at the center of a gas/dust nebula collapse (as opposed to being formed in a protoplanetary disk)?

**Tags:** nebula, brown-dwarf, rogue-planet, red-dwarf, protostar
> **Comments:**
> **username_1**: What do you mean by "Sub-Brown Dwarfs"?  
> **username_2**: *Secretly* more common?  
> **username_3**: Aren’t Sub-brown dwarfs called “planets”?  
> **username_4**: Sub-brown dwarfs also known as planetary-mass brown dwarfs are formed like stars from collapse of a gas cloud, unlike planets which are formed by accretion in a protoplanetary disk. https://en.wikipedia.org/wiki/Sub-brown_dwarf  
> **username_5**: LISA gravitational wave observatory is expected to shed light on the brown dwarf desert/gap https://arxiv.org/abs/1903.02049 and https://arxiv.org/abs/1910.05414 for examples  
> **username_0**: @RBarryYoung, Sub-brown dwarfs are a subset of planets.  Only planets that are formed in the same manner as stars and brown dwarfs can be called sub-brown dwarfs.  Any planet formed in a protoplanetary disc cannot be called a sub-brown dwarf.  
> **username_0**: The Starforge simulations helped provide me with some visual intuition about why brown dwarves might be less common (theoretically). In the simulations, proto-stars in a nebula continue to gravitationally attract more gas until fusion triggers outward stellar winds, which drives away all nearby free gas. This stops the growth of the star. Brown dwarves don't have stellar winds, so there is nothing to stop growth (unless they happen to run out of gas).  https://www.youtube.com/watch?v=qh9TCg-3zus&list=PLtrvxOPz9tAMrMMw7m1I1j4iaXUNB4BK5&index=1  

---

## 3 answers

### Answer by username_1 on 2021-07-01. Score: 11 | Accepted answer

The answer to your first question is (now) fairly simple: No, brown dwarfs are *not* more common than red dwarfs. A crude approximation is that stars (which are indeed mostly red dwarfs) outnumber brown dwarfs 4 or 5 to 1; see, for example, the review article by [Chabrier et al. (2014)](https://arxiv.org/abs/1401.7559). This is supported by extensive surveys done in the 2000s and 2010s, including observations with the WISE telescope; these are sensitive enough to uncover quite faint brown dwarfs.

Empirically, attempts to count stars and brown dwarfs in local volumes strongly suggest that stars outnumber brown dwarfs. For example, [Reylé et al. (2021)](https://arxiv.org/abs/2104.14972) combine *Gaia* observations (sensitive to hydrogen-burning stars and the more massive brown dwarfs) with literature observations of brown dwarfs using IR telescopes (*Spitzer*, *WISE*) to make a census of different objects within 10 pc (33 light years) of the Sun. They find a total of 355 (hydrogen-burning) stars -- including 276 M dwarfs --, 20 white dwarfs (formerly hydrogen-burning), and 85 brown dwarfs (plus 3 more candidates). They do note that there are probably more brown dwarfs waiting to be identified, though these would have to be at the very low-mass (and thus low-luminosity) end. One can still argue that stars outnumber brown dwarfs in our local volume by about three or four to one.

It is true that lower mass stars tend to be more common than higher mass stars. However, this trend becomes weaker for lower masses. The figure below (from the Wikipedia article on the [initial mass function (IMF) of stars](https://en.wikipedia.org/wiki/Initial_mass_function), which tells you how many stars of a given mass are born, as a function of mass) shows several different versions of the IMF. The best current measurements are encoded in either the "Kroupa01" or "Chabrier03" curves, all of which show that the curves flatten -- or even turn over -- for very low masses. This means that if you add up all the brown dwarfs and add up all the stars, you end up with more stars than brown dwarfs.

**Edited to add:** Empirical counts of stars and brown dwarfs in the local volume.

[![enter image description here](https://i.sstatic.net/Psio1.png)](https://i.sstatic.net/Psio1.png)

> **Comments:**
> **username_9**: Your first citation that red dwarfs outnumber brown 4-to-1 uses an IMF not shown in your plot. The Chabrier 03 you show has the peak mass at 8% solar, whereas the 4-to-1 calculation uses 25% solar. Using 8% solar flips things so brown outnumber red 4-to-1. The ratio appears to be highly uncertain.  
> **username_1**: @Xerxes I'm not sure how you're getting 4-to-1 brown-dwarfs to M dwarfs for the Chabrier03 IMF; my integration suggests 1-to-1.4. In any case, I've updated my answer with some notes on observed local counts, which tends to agree with the 4-to-1 stars-to-brown-dwarfs estimate.  
> **username_8**: There are *observations* in open clusters (rather than proposed mass functions) which support the 4 stars to 1 BD figure.  

---

### Answer by username_6 on 2021-07-01. Score: 7

This is an important question to ask about the [initial mass functio](https://en.wikipedia.org/wiki/Initial_mass_function)n of objects in the Galaxy - and the final answer hasn't been cast as it is a matter of research.

Yet, observational data (e.g. see the mass functions for various clusters in [this talk](https://astro.uni-bonn.de/%7Epavel/HLmeeting/2006/talks/thies.pdf)), and simulations in more or less good agreement with that (e.g. [here](https://arxiv.org/pdf/1205.2966.pdf) or [here](https://arxiv.org/pdf/1501.01640.pdf)), seem to indicate that this so-called [brown dwarf desert](https://en.wikipedia.org/wiki/Brown-dwarf_desert) is real and that we talk about fundamentally different formation mechanisms between stars and planets. Yet this doesn't mean that no such objects exist nor do we completely understand the causes for these observational findings. One thing playing a role here could be that there is a lower limit to the [Jeans mass](https://arxiv.org/pdf/2008.06396.pdf) (or rather density) which you will not pass for a single star / brown dwarf by fluctuations in a collapsing gas cloud due to thermodynamics - which seems to be around the Brown dwarf mass.

Just recently there have been attempts to get a better handle on some Brown Dwarfs by help of transit detection (e.g. see [here](https://www.aanda.org/articles/aa/full_html/2019/08/aa35505-19/aa35505-19.html)) which allows to constrain its parameter much better than before.

> **Comments:**
> **username_6**: And I wonder whether reference 3 is written by a certain member of this SE and whether he could thus write a much better answer :)  

---

### Answer by username_4 on 2021-07-01. Score: 3

According to the [wiki](https://en.wikipedia.org/wiki/Sub-brown_dwarf) article on sub-brown dwarfs, the lowest mass object that can form from collapse of gas cloud is about 1 Jupiter mass.

Original source: [Boss, Alan P.; Basri, Gibor; Kumar, Shiv S.; Liebert, James; Martín, Eduardo L.; Reipurth, Bo; Zinnecker, Hans (2003), "Nomenclature: Brown Dwarfs, Gas Giant Planets, and ?"](https://ui.adsabs.harvard.edu/abs/2003IAUS..211..529B/abstract)

> **Comments:**
> **username_2**: How can that be, when Neptune, Uranus and Saturn are also gas giants?  
> **username_4**: Those are planets. They likely formed by accretion in a protoplanetary disk around the sun, not from collapse of gas cloud.  
> **username_7**: @RonJohn if it hasn't been asked already, that might make a good new question.  
> **username_8**: Please cite original work, not wikipedia where possible. It clearly is possible in this case.  

---

