<p>I emailed the authors of the paper, asking whether blue dwarf stars could</p>

<blockquote>
  <p>"become hot enough to pass the thresholds for Type B or Type O"</p>
</blockquote>

<p>and one of them replied:</p>

<blockquote>
  <p>"We use the term 'blue' to mean 'bluer', so that when stars become
  blue, they get hotter than their usual main sequence temperatures. ...
  The point of the paper is that smaller stars get bluer ... But 'blue'
  does not correspond to a particular temperature, and does not mean 'as
  hot as an O star'."</p>
</blockquote>

<p>So it looks like I read the H-R diagram correctly. For the stellar masses represented therein, none of the blue dwarf stars actually reach a high enough surface temperature for type B or O, and white type A stars are the closest any of them will come.</p>

<p>However, that doesn't answer the question for stars with stellar masses not represented in the diagram, for example <span class="math-container">$0.15M_☉$</span>, <span class="math-container">$0.13M_☉$</span> or <span class="math-container">$0.135M_☉$</span>. The authors of the paper didn't run their simulation for these, and there doesn't seem to be enough information in the diagram to make deductions regarding their suface temperature. So until more research is done in this area, the question of whether <em>any</em> blue dwarf stars can actually become blue remains unanswered.</p>

CC BY-SA 4.0
2020-01-12T09:48:13.663Z
2020-01-12T09:48:13.663Z
Astrid_Redfern
<p>The paper <a href="https://onlinelibrary.wiley.com/doi/pdf/10.1002/asna.200510440" rel="noreferrer">"M dwarfs: planet formation and long term evolution"</a> describes blue dwarf stars, a hypothetical next-stage in the lifespan of red dwarf stars within a certain mass range, after which they become white dwarves.</p>

<p>(Hypothetical because the universe is not old enough for any red dwarves to have reached this stage.)</p>

<p>The Hertzsprung Russell diagram on page 917 of this paper, if I've interpreted it correctly (I'd never seen one of these until recently!), shows red dwarves in the 0.14-0.16 solar mass range progressing further away from the "red" end of the spectrum and in the direction of the blue. But it does not actually depict their surface temperature reaching - or indeed exeeding - 9000K (spectral type A, instead of the B or O-type that are normally considered blue enough to justify the name.)</p>

<p><a href="https://i.sstatic.net/MRZv0.png" rel="noreferrer"><img src="https://i.sstatic.net/MRZv0.png" alt="enter image description here"></a></p>

<p>Am I correct that "blue dwarf" stars would not, according to this paper's H-R diagram, actually ever get past "white", and are thus named because they've moved a long way from the red end of the spectrum toward the blue? I have seen different colour charts depict different levels of blueness for the O, B and A types while researching this question, although the majority consensus seems to be that A types are almost entirely white with only a very small amount of blue.</p>

<p>(The same Hertzsprung-Russell diagram is also shown on page 424 of the 1997 paper <a href="https://iopscience.iop.org/article/10.1086/304125/pdf" rel="noreferrer">"The End of the Main Sequence"</a>, if that helps at all.)</p>

CC BY-SA 4.0
2019-11-21T21:51:24.187Z
Interesting question ! Can you edit your question to include a link to the astro-ph or other public version of the paper and/or include the relevant diagram in the question ?
astrosnapper
CC BY-SA 4.0
2019-11-21T22:00:00.800Z
@astrosnapper That's a very good idea - I'm kicking myself for not doing so from the start! Links to non-paywalled, publicly-downloadable PDFs have been added.
Astrid_Redfern
CC BY-SA 4.0
2019-11-21T22:04:28.510Z
@astrosnapper A .png of the diagram has also been added.
Astrid_Redfern
CC BY-SA 4.0
2019-11-21T22:47:08.667Z
@antispinwards That's exactly what I was wondering.
Astrid_Redfern
CC BY-SA 4.0
2019-11-21T22:59:12.630Z
There's a precedent in H-R diagrams of using "blue" in reference to stars that shift bluewards without actually looking blue: the [blue loop](https://en.wikipedia.org/wiki/Blue_loop).
PM 2Ring
CC BY-SA 4.0
2019-12-20T16:04:05.610Z
A belated update - I emailed the authors of the paper, and one of them has replied.  
"We use the term 'blue' to mean 'bluer', so that when stars become 
blue, they get hotter than their usual main sequence temperatures. ... The point of the paper is that smaller stars get bluer ... But 'blue' does not correspond to a particular temperature, and does not mean 'as hot as an O star'.".  
He CCed the other authors in his answer, so I'll wait a bit in case one of them has anything more to add, but it looks like I'm going to be posting and accepting this as an answer to my own question.
Astrid_Redfern
CC BY-SA 4.0
2019-12-20T16:10:38.087Z
Sorry if the above's hard to read - I followed the instructions in Comment Formatting but couldn't get the linebreaks to show.
Astrid_Redfern
CC BY-SA 4.0
2020-01-12T09:34:00.627Z
I held off turning the above comment into an answer for a while - I thought, they might not be reading emails over the Christmas period, give them time - but I think by now I'm not going to get any follow-up replies. So I'm preparing the answer now.
Astrid_Redfern
<star><stellar-evolution><white-dwarf><red-dwarf><dwarf-star>
The colour of blue dwarf stars
Astrid_Redfern
# The colour of blue dwarf stars

(Asked by: username_0 on 2019-11-21)

The paper ["M dwarfs: planet formation and long term evolution"](https://onlinelibrary.wiley.com/doi/pdf/10.1002/asna.200510440) describes blue dwarf stars, a hypothetical next-stage in the lifespan of red dwarf stars within a certain mass range, after which they become white dwarves.

(Hypothetical because the universe is not old enough for any red dwarves to have reached this stage.)

The Hertzsprung Russell diagram on page 917 of this paper, if I've interpreted it correctly (I'd never seen one of these until recently!), shows red dwarves in the 0.14-0.16 solar mass range progressing further away from the "red" end of the spectrum and in the direction of the blue. But it does not actually depict their surface temperature reaching - or indeed exeeding - 9000K (spectral type A, instead of the B or O-type that are normally considered blue enough to justify the name.)

[![enter image description here](https://i.sstatic.net/MRZv0.png)](https://i.sstatic.net/MRZv0.png)

Am I correct that "blue dwarf" stars would not, according to this paper's H-R diagram, actually ever get past "white", and are thus named because they've moved a long way from the red end of the spectrum toward the blue? I have seen different colour charts depict different levels of blueness for the O, B and A types while researching this question, although the majority consensus seems to be that A types are almost entirely white with only a very small amount of blue.

(The same Hertzsprung-Russell diagram is also shown on page 424 of the 1997 paper ["The End of the Main Sequence"](https://iopscience.iop.org/article/10.1086/304125/pdf), if that helps at all.)

**Tags:** star, stellar-evolution, white-dwarf, red-dwarf, dwarf-star
> **Comments:**
> **username_1**: Interesting question ! Can you edit your question to include a link to the astro-ph or other public version of the paper and/or include the relevant diagram in the question ?  
> **username_0**: @astrosnapper That's a very good idea - I'm kicking myself for not doing so from the start! Links to non-paywalled, publicly-downloadable PDFs have been added.  
> **username_0**: @astrosnapper A .png of the diagram has also been added.  
> **username_0**: @antispinwards That's exactly what I was wondering.  
> **username_2**: There's a precedent in H-R diagrams of using "blue" in reference to stars that shift bluewards without actually looking blue: the [blue loop](https://en.wikipedia.org/wiki/Blue_loop).  
> **username_0**: A belated update - I emailed the authors of the paper, and one of them has replied.   "We use the term 'blue' to mean 'bluer', so that when stars become  blue, they get hotter than their usual main sequence temperatures. ... The point of the paper is that smaller stars get bluer ... But 'blue' does not correspond to a particular temperature, and does not mean 'as hot as an O star'.".   He CCed the other authors in his answer, so I'll wait a bit in case one of them has anything more to add, but it looks like I'm going to be posting and accepting this as an answer to my own question.  
> **username_0**: Sorry if the above's hard to read - I followed the instructions in Comment Formatting but couldn't get the linebreaks to show.  
> **username_0**: I held off turning the above comment into an answer for a while - I thought, they might not be reading emails over the Christmas period, give them time - but I think by now I'm not going to get any follow-up replies. So I'm preparing the answer now.  

---

## 1 answers

### Answer by username_0 on 2020-01-12. Score: 4 | Accepted answer

I emailed the authors of the paper, asking whether blue dwarf stars could

> "become hot enough to pass the thresholds for Type B or Type O"

and one of them replied:

> "We use the term 'blue' to mean 'bluer', so that when stars become
> blue, they get hotter than their usual main sequence temperatures. ...
> The point of the paper is that smaller stars get bluer ... But 'blue'
> does not correspond to a particular temperature, and does not mean 'as
> hot as an O star'."

So it looks like I read the H-R diagram correctly. For the stellar masses represented therein, none of the blue dwarf stars actually reach a high enough surface temperature for type B or O, and white type A stars are the closest any of them will come.

However, that doesn't answer the question for stars with stellar masses not represented in the diagram, for example $0.15M\_☉$, $0.13M\_☉$ or $0.135M\_☉$. The authors of the paper didn't run their simulation for these, and there doesn't seem to be enough information in the diagram to make deductions regarding their suface temperature. So until more research is done in this area, the question of whether *any* blue dwarf stars can actually become blue remains unanswered.


---

