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[[File:Sciences humaines.svg|40px]] This article was the subject of a Wiki Education Foundation-supported course assignment, between <span class="mw-formatted-date" title="2019-01-07">7 January 2019</span> and <span class="mw-formatted-date" title="2019-04-25">25 April 2019</span>. Further details are available [[Wikipedia:Wiki_Ed/Oklahoma_Christian_University/Comp_II_(Spring_2019)|on the course page]]. Student editor(s): [[User:KatepaImer|KatepaImer]].

==Metallicity==
It seems to me that if we have not observed any red dwarf stars with zero metal content, then we have indeed observed red dwarf stars that have moved off the main sequence and we are still left with the puzzle of determining the precise age of the universe. About all we can say for certain is that the universe should be much older than the estimates that are popular at the moment.
:Red dwarf stars are so common that we haven't even bothered to study most of the ones we've discovered. If we haven't discovered a red dwarf of Population III, it's probably because we haven't looked hard enough. If low-mass stars formed during that age of the Universe, then both red and orange dwarfs with no metals should exist. No star of less than 80 percent of the mass of the Sun has evolved off the main sequence yet. [[user:Jsc1973]]

The reason I bring this up is because I cannot imagine how you find a red dwarf that has gone cold. It seems unlikely that they would become white dwarfs harboring degenerate matter. This is a case of an absence of something indicating a condition we have failed to properly conisider.

== Giant dwarfs ==

I disagree with this statement:
{{tmbox
|image = none
|text = Red dwarfs never initiate helium fusion and so cannot become red giants
}}
Red giants, at least as expected with Sun-like stars, occur ''before'' the initiation of helium fusion, with shell hydrogen fusion. Although it might take more-then-the-current-age-of-the-Universe for red dwarfs to reach the point of having an inert helium core, I could imagine this state of affairs, at least with the bigger end of red dwarfs. Does anyone have any better information? [[User:Joffan|Joffan]] 19:02, 16 September 2005 (UTC)

:IIRC, red dwarves have convection cells going all the way down to the core, so there is no shell hydrogen fusion. One of the reasons they live so long is that most of the hydrogen in them reaches the core at some point, so the core is never "inert" until they die. [[User:Linguofreak|Linguofreak]] 04:42, 10 April 2006 (UTC)


At the begining of the Main Sequence red dwarfs are fully convective. As a red dwarf ages the hydrogen to helium ratio decreases throughout the star. This forces the temperature of the core up to maintain the rate of fusion. At some point this causes a radiative shell to develop between a convective core and a convective exterior. The hydrogen outside the core is no longer available for fusion and the evolution proceeds rapidly. What happens next depends upon mass.
:For masses greater than about 0.25 to 0.20 solar masses, fusion in the core proceeds until the hydrogen is exhausted. The core contracts, heats up and the star turns off the main sequence. It becomes a red giant under-going hydrogen shell burning around an inert helium core. However the star does not reach a core temperatures sufficient to undergo the helium flash, fusion slows and ultimately ends.

:For lower masses the core of the star is already partially supported by degenerate electron pressure. As a result of this, there is a limit to the amount the core can contract to maintain the fusion rate. So that as hydrogen is exhausted in the core fusion throughout the star slows and dies. The low mass M-dwarf never becomes a red giant.

Disclaimer, much of what I have said above occurs on timescales greater than the age of the Universe, so is completely untestable. Thus this is more speculation than rigorous science.
--[[User:Ealdian|Ealdian]] 14:26, 17 August 2006 (UTC)

Actually, if a red dwarf has a mass greater than 0.4 mass of the Sun, not all of the star’s region is convection zone and it could become a red giant. —-[[User:Anonymous|Anonymous]] 17:38, 29 June 2019  <!-- Template:Unsigned IP --><small class="autosigned">—&nbsp;Preceding [[Wikipedia:Signatures|unsigned]] comment added by [[Special:Contributions/2402:800:61B1:773A:1464:BA3B:13D2:A65D|2402:800:61B1:773A:1464:BA3B:13D2:A65D]] ([[User talk:2402:800:61B1:773A:1464:BA3B:13D2:A65D#top|talk]]) </small> <!--Autosigned by SineBot-->

== Population III stars. ==

Stars of extremely high mass that burned out quickly, by cosmological standards, and thereby created all the metals needed for the current crop of Population II and Population I stars. Shouldn't this have left us with a very high number of neutron stars, magnetars, and black holes? Wouldn't the consequences of having a large number of such objects around be rather serious?

Here, I am not criticizing Wikipedia as this seems to be an accurate exposition of current theory. Nevertheless, I do have serious misgivings about the theory. Granted, Astronomers, Astrophysicists, and Comologists need a theory to work with and from, but they seem terribly cocksure at times.

Quoting the article on Pop III stars here, because I cannot get the talk tab to work on that article:

"If these stars were able to form properly, their lifespan would be extremely short, certainly less than one million years. As they can no longer form today, viewing one would require us to look to the very edges of the observable universe. (Since the time it takes light to reach Earth from great distances is extremely long, it is possile to see "back in time" by looking farther away.) Seeing this distance while still being able to resolve a star could prove difficult even for the James Webb Space Telescope."

If the theory concerning these putative stars is in any way correct, then JWST should be able to view entire galaxies of such stars, yes? The spectra of nearly all the stars should all be very nearly the same, depending upon the age of the putative galaxies of Pop III stars. In fact I would expect the spectra of such young galaxies to fall into "bins" according to their ages. A galaxy only one million years old should be easily distinguishable from one that is slightly older than one million years and so on until all the Pop III stars have had time to burn out. Metalicity galaxy wide should increase with age in almost stair-step fashion.

It amazes me, by the way, that something around one percent or less of elements heavier than helium can have such profound effects on stellar size. Current counts suggest that the overwhelming majority of Pop II and Pop I stars are K to M class dwarfs. Why the anticipated paucity of such stars in Pop III? Simply because we have not found any such stars that have turned off the main sequence?

Personally, I think it is more likely that we have not found them because they are dim and we have not devoted enough instrument time to look for them. But, then again, perhaps the black holes gobbled them up.

[[User:70.116.68.198|70.116.68.198]] 06:56, 1 January 2006 (UTC)Don Granberry.

Maybe red dwarfs are population llll stars([[Population lll stars]] with carbon)  <small><span class="autosigned">—Preceding [[Wikipedia:Signatures|unsigned]] comment added by [[User:Alexrybak|Alexrybak]] ([[User talk:Alexrybak|talk]] • [[Special:Contributions/Alexrybak|contribs]]) 17:16, 22 May 2011 (UTC)</span></small><!-- Template:Unsigned --> <!--Autosigned by SineBot-->

== More on Population III Stars ==

Here is a very useful link:

http://www.journals.uchicago.edu/ApJ/journal/issues/ApJ/v540n1/50350/50350.html

Somewhere along the way, their simulation runs must have butted heads with Xeno of Elea. They assume the existence of "dark matter" and a considerably less than homogenous cloud structure in the "early universe."

There is no suggestion that any non-linear, self-iterative processes were considered. Such large clouds of gasses would necessarily be affected by such processes. Quoting the above linked article:

"What will be the fate of the collapsing core? Within the core the number densities increase from 105 to 108 cm-3. For densities &gsim;108 cm-3, however, three-body formation of H2 will become the dominant formation mechanism, transforming all hydrogen into its molecular form (Palla et al. 1983). Our chemical reaction network does not include this reaction, and the solution cannot be correct at r &lsim; 0.1 pc. The most interesting effect of the three-body reaction is that it will increase the cooling rate by a factor of ∼103, leading to a further dramatic density enhancement within the core. This will decrease the dynamical timescales to &Lt;100 yr, effectively decoupling the evolution of the fragment from the evolution of its host primordial molecular cloud. Therefore, it is a firm conclusion that only the gas within these cores can participate in Population III star formation."

The model used relies non-local thermodynamic equilibrium and this can be problematic.

http://www.physics.usyd.edu.au/astron/iau189/toc-posters.ps


Also, the one description of the nucleosynthesis process in Population III stars that I could access assumes that the stars are not rotating.

http://www.journals.uchicago.edu/ApJ/journal/issues/ApJ/v567n1/54373/54373.text.html?erFrom=-7768877433592011253Guest


The upshot is that we appear to be placing a wee bit too much faith in a computing model limited by computing resources, particularly when it is claimed that only very large stars (30 to 1000 solar masses) were made during this period of cosmological history and that none of those stars were in rotation.

While this IS a good working theory on which to foot further investigations, the investigators seem to be entirely too eager to comply with pre-conceived notions. In court they would be accused of "assuming facts not in evidence." Rather than being an effort to discover the nature of stars that formed during the early periods of the universe, assuming the universe had an "early period", this seems to be an attempt to shore up a problem ridden model of the universe.

The current cosmological model may one day be shown to be correct, but dogmatic adherence to it prior to such a demonstration strikes me as being a very poor procedure. While a sincere search for very old red dwarfs or K stars of Population III origin would be arduous, it should nevertheless be carried out.

[[User:70.116.68.198|70.116.68.198]] 17:29, 1 January 2006 (UTC)Don Granberry

== Carbon ==

Do Red Dwarfs have any carbon within them? [[User:Zachorious|Zachorious]] 05:09, 31 July 2006 (UTC)

All observed red dwarfs contain carbon. Carbon is in the top 5 most abundant elements in the Universe. It is likely that the only red dwarfs which contain no carbon belong to Population III. If such stars still exist they are may have accreated material from the interstellar medium or a companion star and so contain at least a tiny amount of carbon. You may be interested in the extremely iron deficient star HE 1327-2326, which has an iron to hydrogen ratio of 1/250000 of the solar value.

Carbon?Aha!Carbon in outer layers,NOT IN THE CORE!  <small><span class="autosigned">—Preceding [[Wikipedia:Signatures|unsigned]] comment added by [[User:Alexrybak|Alexrybak]] ([[User talk:Alexrybak|talk]] • [[Special:Contributions/Alexrybak|contribs]]) 17:08, 22 May 2011 (UTC)</span></small><!-- Template:Unsigned --> <!--Autosigned by SineBot-->

== Nucleosynthysis ==

This statement does not seem right to me
{{tmbox
|image = none
|text = Since a low mass star fuses hydrogen in the presence of metals, then an early protostar of such a low mass devoid of metals would not 'go nuclear', it would simply sit around as a clump of gas until more material came along.
}}
I assume 'fuses hydrogen in the presence of metals' refers to the carbon-nitrogen-oxygen (CNO) cycle in which fusion is catalysed by C,N and O. However, the CNO cycle does not become efficient until temperatures in excess of around 16 million Kelvin are reached. On the Main Sequence, such temperatures are only reached in stars of greater than about 1 solar mass. For low mass stars (and the Sun) the main fusion reactions which occur are those of the proton-proton (PP) chains. The PP-chains do not require the presence of metals, so Population III red dwarfs can exist.

== The British TV programme ==

I believe it was a children's television programme.  I suggest we change the link to say:  "For the British children's television programme from the 1980s..." - <span style="font-size: smaller;" class="autosigned">— Preceding [[Wikipedia:Signatures|unsigned]] comment added by [[Special:Contributions/138.37.7.247|138.37.7.247]] ([[User talk:138.37.7.247|talk]]) </span><!-- Template:Unsigned IP -->

:Erm, no, we shouldn't, as it wasn't. --[[User:NeilTarrant|Neo]] 22:11, 1 February 2007 (UTC)

::Okay, but I can't find anywhere that states it's not a children's programme.  Could we please then highlight that it's an adult programme, and provide some kind of reference to support this detail?  Thanks. <small>—The preceding [[Wikipedia:Sign your posts on talk pages|unsigned]] comment was added by [[Special:Contributions/138.37.107.212|138.37.107.212]] ([[User talk:138.37.107.212|talk]]) 20:00, 4 February 2007 (UTC).</small><!-- HagermanBot Auto-Unsigned -->

:::I think we shouldn't because I'm not confident that you are acting in good faith here. Given the time the programme was shown (I'm guessing you are British given the way you've spelt programme) was post watershed, and the content was quite clearly adult themed I don't see how anyone could mistake the show for a children's programme. --[[User:NeilTarrant|Neo]] 20:50, 11 February 2007 (UTC)

:::The shows on DVD are certificate 12.  Definitely NOT a children's programme which are all certificate PG or U. [[User:QuiteUnusual|QuiteUnusual]] 22:21, 11 February 2007 (UTC)

::::The main Red Dwarf television page now emphasises that Red Dwarf was adult-oriented, to avoid confusion.  Somebody may decide to make the same change here, but I'm not going to suggest either way. <small>—The preceding [[Wikipedia:Sign your posts on talk pages|unsigned]] comment was added by [[Special:Contributions/86.142.211.223|86.142.211.223]] ([[User talk:86.142.211.223|talk]]) 20:48, 12 February 2007 (UTC).</small><!-- HagermanBot Auto-Unsigned -->

::::Further to this comment I notice that this issue is considered "resolved" by the article for the television programme (see the discussion page), so we may as well put "adult-oriented" here too.  I have made the change - hope this keeps everyone happy.

:::::While I wasn't the person who removed the 'adult oriented' line, I must say that I agree with it having been removed - this is not a page about the show; in fact we don't need to say anything about the show here! I suggest we replace the whole thing with "For the <strike>adult-oriented British comedy series from the 1980s and 1990s</strike>television programme, see [[Red Dwarf]]."  - this is akin to links on the page '[[White dwarf]]' which lists
:::::* For the magazine, see [[White Dwarf (magazine)]].
:::::* For the song "White Dwarf" by a-ha, see ppAnalogue]].
:::::* For the movie "White Dwarf", see [[White Dwarf (movie)]].
:::::And indeed the [[Red Dwarf]] page which has simply 'For the type of star, see [[Red dwarf]].'
:::::In fact, I'm going to be bold and just make the change myself. -- [[User:NeilTarrant|Neo]] 20:17, 25 February 2007 (UTC)
::::::Following that, should the RD TV article/link perhaps be "Red Dwarf (TV show)"? Right now all that separates this page from that one is the capitalisation of "d/Dwarf", which I can't help but think of as very bad practice. [[Special:Contributions/193.63.174.10|193.63.174.10]] ([[User talk:193.63.174.10|talk]]) 11:49, 21 September 2009 (UTC)

::::::I think the tv show was actually for adults that acted like children, hence the confusion. [[User:Rich.lewis|Rich.lewis]] 01:18, 25 April 2007 (UTC)
:::::::In opposition, I prefer to apply Hanlon's Razor... [[Special:Contributions/193.63.174.10|193.63.174.10]] ([[User talk:193.63.174.10|talk]]) 11:49, 21 September 2009 (UTC)

== Life on red dwarf planet ==

Is life probable on planet that revolves around a red dwarf ? <small>—The preceding [[Wikipedia:Sign your posts on talk pages|unsigned]] comment was added by [[Special:Contributions/64.18.179.229|64.18.179.229]] ([[User talk:64.18.179.229|talk]]) 20:17, 2 March 2007 (UTC).</small><!-- HagermanBot Auto-Unsigned -->

:There is a renewed interest in the possibility of habitable planets of red dwarf stars.  Several papers on the subject appear in a new special issue of Astrobiology.  [[User:Vegasprof|Vegasprof]] 07:43, 9 April 2007 (UTC)

:The article assumes plant life (and photosynthesis). On Earth, there's life that lives deep under the sea at thermal vents, that doesn't depend on any sunlight. http://en.wikipedia.org/wiki/Deep_sea_vents#Biological_communities It seems tidal heating could keep thermal vents active http://en.wikipedia.org/wiki/Io_(moon)#Orbit_and_rotation
:Interestingly, does this mean that a non-star could still support life? (cool!) [[Special:Contributions/lionfish0|lionfish0]] ([[User talk:lionfish0|talk]]) 18:06, 31 August 2009 (UTC) (lionfish0)

I am probably doing this wrong as I have never done anything to a Wiki, but I was curious in this article how it is mentioned that one of the difficulties in supporting life around a Red Dwarf was due to the fact that little to no UV radiation was emitted by such a star. However in this article from Space.com "Can Life Thrive Around A Red Dwarf Star" http://www.space.com/scienceastronomy/090409-sm-reddwarf-life.html
It states that the difficulty is that UV radiation can be 100-10,000 more than normal. Well, if there were little to no UV radiation than 10,000 times more than almost none shouldn't necessarily be so big a concern. I feel like this entire article is full of factual errors, just based on scanning this discussion page and reading articles from more reputable sources. This is a much more glaring error than say the artist rendition error mentioned above. Someone who knows more should really fix this before misinformation can confuse too many people.  <span style="font-size: smaller;" class="autosigned">—Preceding [[Wikipedia:Signatures|unsigned]] comment added by [[Special:Contributions/184.56.26.53|184.56.26.53]] ([[User talk:184.56.26.53|talk]]) 14:53, 10 December 2010 (UTC)</span><!-- Template:UnsignedIP --> <!--Autosigned by SineBot-->

There's all sorts of issues in this area. Tidal Locked planets are still being described as if the have very thin to no atmospheres, which might be an issue for life, since that's the only way to get massive temperature differences. Since we have Venus to see what happens when you have a very slow rotation and a thick atmosphere. At least it's been given the "could" designation.  <!-- Template:Unsigned IP --><small class="autosigned">—&nbsp;Preceding [[Wikipedia:Signatures|unsigned]] comment added by [[Special:Contributions/68.107.138.23|68.107.138.23]] ([[User talk:68.107.138.23#top|talk]]) 19:23, 18 May 2018 (UTC)</small> <!--Autosigned by SineBot-->

== link color? ==

Why are the links to other articles in this page red? [[User:140.198.172.119|140.198.172.119]] 17:52, 10 May 2007 (UTC)
:I can only see one [[red link]] in the article - maybe it was the computer you were using having odd internet settings? --[[User:NeilTarrant|Neo]] 18:00, 10 May 2007 (UTC)

== When they leave the main sequence ==

Hi, what happens when a red dwarf runs out of hydrogen? Are they massive enough to swich to helium fusion and become red giants, as the sun will in 5 thousand million years <small>(sorry, still reluctant to adopt the short scale)</small>? Yeah, I know no the universe is too young for a red dwarf to have run out of fuel anyway, but I am just curious... [[User:Steinbach|Steinbach <small>(fka Caesarion)</small>]] 15:21, 12 May 2007 (UTC)

The article on [[Stellar evolution#Low-mass stars|stellar evolution]] states that 'A star of less than about 0.5 solar mass will never be able to fuse helium even after the core ceases hydrogen fusion' however apparently if the core is not fully convective - i.e. if there are stratified layers inside the star then 'it will develop into a red giant ... but never fuse helium as they do; otherwise, it will simply contract until electron degeneracy pressure halts its collapse, thus directly turning into a white dwarf.' --[[User:NeilTarrant|Neo]] 21:18, 12 May 2007 (UTC)

== Steller Evolution ==

I thought that the [[White dwarf]] stars gradually cool to become [[Red dwarf]] stars, on their way to evolving into [[Black dwarf]] stars... is that true, or are these completely separate stars, like [[Brown dwarf]] and [[Sub-brown dwarf]] stars? (i'm asking becuase i was taught that stars go from white to red to black in grade 5, but i was always skeptical of that. <span style="border: 2px solid #330000; text-align:center; background: #C0C0C0; text-color: #DDDDDD; link: #A0522D; vlink: #000000"> '''[[User:RingtailedFox|RingtailedFox]]''' • [[User talk:RingtailedFox|'''Talk''']] • [[Special:Contributions/RingtailedFox|'''Stalk''']]'''</span> 17:18, 12 May 2007 (UTC)

:Yes and no - Yes, white dwarves will cool and emit radiation in the red region - see [[White dwarf#Radiation and cooling|here]], bt they're still called white dwarves, not red dwarves to avoid confusion with the stars presumably. --[[User:NeilTarrant|Neo]] 21:18, 12 May 2007 (UTC)

::White dwarves are partially collapsed stars comprised of degenerate matter (not neutronium however) - they are the final stage after (elderly) red giants of roughly the same mass as our sun.  A red dwarf masses much less and never collapses because its mass can be supported by interatomic forces.  Although white dwarves will eventually cool and radiate longer wavelengths, the universe isn't old enough for white dwarves to have turned red yet!  When that time comes, two stars of these types might have roughly the same size, color, and temperature, but would still be totally different.  (Apparently all kinds of strange ideas are taught in elementary and secondary science classes in America these days.  It was not always so... ) The different kinds of star are mostly determined by mass.  The larger, the brighter and shorter-lived, and the more likely to turn into a bizarre object.  The smaller, the darker and longer-lived.  Please read up on this if you are interested.[[User:Vendrov|Vendrov]] 07:53, 21 September 2007 (UTC)

== Planets ==

SOmeone more knowledgeable than me needs to re-add the Planets section. I just blanked it because other than the heading '''Planets''' the section was empty except for the words, "Eat anus." [[User:Basejumper2|Basejumper2]] 12:54, 25 October 2007 (UTC)

:I changed the section marked "Detection" to "Planets", because the section actually discussed only detecting plants (or rather, listed recently detected planets) rather than detecting Red Dwarfs. --[[User:Noclevername|Noclevername]] ([[User talk:Noclevername|talk]]) 01:24, 5 March 2008 (UTC)

I’m fine with this change. It’s correct since the detecting went mostly for plants. --[[User:DavidD4scnrt|DavidD4scnrt]] ([[User talk:DavidD4scnrt|talk]]) 06:59, 10 April 2008 (UTC)

The planets here are only the new ones from 2005 and later. There are several planets orbiting red dwarfs, so I think we should create an article called: [[List of red dwarf planetary systems]] or something. I'll try to gather up enough info for it. --[[User:UltimateDarkloid|UltimateDarkloid]] ([[User talk:UltimateDarkloid|talk]]) 12:23, 15 September 2008 (UTC)

Gliese 370 b is mentioned at the end of the planets section but Gliese 370 isn't an M dwarf, or even a late k dwarf, it's a K5V and so doesn't that make Gliese 370 an orange dwarf star? Perhaps, if you want to mention it anywhere it should maybe be put into the [[K-type main-sequence star]] article.  <span style="font-size: smaller;" class="autosigned">— Preceding [[Wikipedia:Signatures|unsigned]] comment added by [[Special:Contributions/86.128.86.65|86.128.86.65]] ([[User talk:86.128.86.65|talk]]) 03:00, 24 March 2012 (UTC)</span><!-- Template:Unsigned IP --> <!--Autosigned by SineBot-->
: I removed the paragraph on Gl. 370 from this article. Thanks for the catch. Regards, [[User:RJHall|RJH]] ([[User_talk:RJHall|''talk'']]) 21:30, 16 April 2012 (UTC)

== WikiProject class rating==
This article was automatically assessed because at least one WikiProject had rated the article as start, and the rating on other projects was brought up to start class. [[User:BetacommandBot|BetacommandBot]] 10:02, 10 November 2007 (UTC)

== Too red, too red ==

That "artist's conception" of a red dwarf is simply far too red.  An ordinary incandescent tungsten light bulb radiates at about half the temperature of a red dwarf.  Its light is a soft yellow-orange-white against daylight and comparatively nearly white at night.  Red dwarf stars just aren't that ... ''red''.  [[User:68Kustom|68Kustom]] ([[User talk:68Kustom|talk]]) 15:39, 5 September 2008 (UTC)

Depends on the [[Spectral type]] and [[Mass|mass]] of the Red Dwarf. There are those that are dim and look almost like [[Brown dwarf|Brown Dwarfs]] and those that are slightly orangish, --[[User:UltimateDarkloid|UltimateDarkloid]] ([[User talk:UltimateDarkloid|talk]]) 12:23, 15 September 2008 (UTC)

: They'd still be bright yellow-orange-white, not dark ember/ruby red as depicted on this page. But it's part of one of the most far-reaching misconceptions in stellar astronomy: the actual colour of stars. I mean, try to argue that Procyon isn't yellow-white (it's bluish-white) ... heck, the latest ''Astronomy'' mag has pictures of Capella (white) and Betelgeuse (yellow).  <small><span class="autosigned">—Preceding [[Wikipedia:Signatures|unsigned]] comment added by [[User:68Kustom|68Kustom]] ([[User talk:68Kustom|talk]] • [[Special:Contributions/68Kustom|contribs]]) 05:05, 31 December 2008 (UTC)</span></small><!-- Template:Unsigned --> <!--Autosigned by SineBot-->
:: I agree with your point. The red coloration is primarily based upon how the human eye perceives the hue of a point light sources at night. [http://outreach.atnf.csiro.au/education/senior/astrophysics/photometry_colour.html This article] has a good discussion on the topic, while [http://www.vendian.org/mncharity/dir3/starcolor/ here] is a table of star colors based upon their blackbody temperature. As an example, I attempted to provide a more realistic appearance of a red dwarf in the [[:File:Alpha centauri size.png]] image, with base colors based on temperature and luminosity showing  greater saturation toward the center of the star (the opposite of limb darkening, I suppose). :-) The [[:File:Mira 1997.jpg]] image shows something comparable for an M7 class star, although I'm not sure if the colors have been adjusted.&mdash;[[User:RJHall|RJH]] ([[User_talk:RJHall|''talk'']]) 20:52, 12 November 2009 (UTC)

:::1. You all know: "artists conception",
:::2. 68Kustom, the misconception comes from the 19th century studies of star colors without spectroscopy before color photography: my private experience with trying to observe the colors of the stars by naked eye and binoculars indicate that the names describe a weak nuance deviation from clean white, so that stars that are actually orangeish pink (fex Betelgeuze) are called "red" and stars that are actually bluish white (fex Rigel) are called "blue". So "red" should be translated to "pink" or "orangeish pink". [[User:Rursus|Rursus]] dixit. ([[User talk:Rursus|<span style="color: red; background: #FFFF80"><sup>m</sup><u>bork<sup>3</sup></u></span>]]!) 08:40, 20 November 2010 (UTC)
:::3. The image is PD, so remixing it to a realistic color would be acceptable and desired. [[User:Rursus|Rursus]] dixit. ([[User talk:Rursus|<span style="color: red; background: #FFFF80"><sup>m</sup><u>bork<sup>3</sup></u></span>]]!) 08:49, 20 November 2010 (UTC)

==What is a red dwarf?==
I think the general conception of the noun phrase "red dwarf star" gives the impression that "red dwarf stars" are stars that are very tiny and red. Not so. I believe "red dwarf star" are '''low mass stars that are fully convective and not giants''', i.e. only fusing hydrogen to helium, not helium to carbon (nor oxygen). They're residing on the lower "red" end of the Hertzsprung-Russell diagram, which is the lower red extension of the main sequence. They're pinkish and orangeish because of low surface temperature, which translates to "red" in astronomy jargon. [[User:Rursus|Rursus]] dixit. ([[User talk:Rursus|<span style="color: red; background: #FFFF80"><sup>m</sup><u>bork<sup>3</sup></u></span>]]!) 08:49, 20 November 2010 (UTC)

I was curious as to the difference between [[Red dwarfs]], [[Brown dwarfs]] and [[White dwarfs]].  Each of the three articles rarely or never mention the others, although it's natural to assume there's a similarity.  From what I've read of the three:

• Red dwarfs are full-on  stars, just small, maybe can't do helium fusion.

• Brown dwarfs are smaller still, can't even fuse hydrogen, but can participate in some lame fusion reactions, if they're lucky.  Their surface temperatures range down to room temperature!  Their sizes range down to gas giant planets.

• White dwarfs are supernova remnants; totally different from the other two.  They often have surface temperatures comparable to stars (hence 'white') from residual heat; can't do fusion.  If they get bigger, 1.44M<sub>☉</sub>, they become neutron stars  (after maybe a supernova).  (And neutron stars similarly become black holes beyond 3M<sub>☉</sub>.)

I'd prefer if a professional could supply and correct these guesses of  mine in the article, maybe a separate section.  Also the other two articles.
[[User:OsamaBinLogin|OsamaBinLogin]] ([[User talk:OsamaBinLogin|talk]]) 20:35, 11 May 2022 (UTC)

: (I’m not an astronomer.) White dwarfs: OK. Red dwarfs: OK. Brown dwarfs: Not being a scientific term, I’m not sure what “lame” means. As I understand it, the distinction between a planet and a brown dwarf is that the brown dwarf can fuse deuterium and possibly lithium at the time of its birth; a planet cannot. Therefore, not “if they are lucky”; rather, “always at time of formation”. As I understand it, there’s a conflict between the theoretics and the empirics of red dwarfs verses brown dwarfs. (That is, aside from the fact that term “red dwarf” is not well defined.) As you note, red dwarfs are always capable of fusing protium (= ¹H). However, it’s very difficult to distinguish the bottom end of the red dwarf range from brown dwarfs because their spectra can be identical to brown dwarfs. Therefore we may not be able to distinguish whether a given L or M dwarf is a red dwarf versus a brown dwarf.
: As far as editing the articles goes, I guess I see everything I expect to see in them already. [[User:Strebe|Strebe]] ([[User talk:Strebe|talk]]) 23:50, 11 May 2022 (UTC)

: Something doesn't make sense in the sentence "..less massive objects, as they age, would increase their surface temperatures and luminosities becoming blue dwarfs and finally white dwarfs." My understanding is that white dwarfs have already been observed and blue dwarfs haven't had time to develop (because universe is too young). Is it maybe "white dwarfs and finally blue dwarfs"?  <!-- Template:Unsigned IP --><small class="autosigned">—&nbsp;Preceding [[Wikipedia:Signatures|unsigned]] comment added by [[Special:Contributions/69.204.170.117|69.204.170.117]] ([[User talk:69.204.170.117#top|talk]]) 14:45, 10 February 2023 (UTC)</small> <!--Autosigned by SineBot-->
::Just because some stars have formed white dwarfs, which we observe, doesn't mean that others won't form white dwarfs in the far future.  We haven't observed any post-blue-dwarf white dwarfs.  [[User:Lithopsian|Lithopsian]] ([[User talk:Lithopsian|talk]]) 15:10, 10 February 2023 (UTC)

:: There are different ways of becoming a white dwarf, in other words. The path of a red dwarf evolving into a blue or white dwarf is one that has not happened yet.[[User:Strebe|Strebe]] ([[User talk:Strebe|talk]]) 17:51, 10 February 2023 (UTC)

== Grammar in the lead ==

From Earth, ''no red dwarfs'' '''are''' visible to the naked eye.

Let's replace the subject "no red dwarfs" with "none"
:From Earth, ''none'' '''are''' visible to the naked eye.

None is not simply a singular combination of "no one". It can act as a plural for "not any". In this context, the subject (red dwarfs) is plural, and appears as plural in the sentence directly preceding. Therefore, the proper usage is "none ''are''" which is plural. The user asked me to look it up, and I did before they told me and found several sites:
[http://grammar.quickanddirtytips.com/none-is-or-none-are.aspx] [http://motivatedgrammar.wordpress.com/2009/01/08/none-is-none-are-grammar-according-to-clarkson/] [http://alt-usage-english.org/excerpts/fxnoneis.html] [http://www.grammarmudge.cityslide.com/articles/article/1026513/9903.htm]
The first time I read that sentence I knew it didn't sound right, and I was correct. "None is" is used for singular subject (Not one red dwarf IS visible to the naked eye) but in this case the preceding used plural, therefore it is No red dwarfs ARE visible to the naked eye. [[User:Cadiomals|Cadiomals]] ([[User talk:Cadiomals|talk]]) 15:33, 28 September 2012 (UTC)

:The question is not whether "none are" ''can'' be correct; the question is whether the sentence is correct as it was written and intended. You cited purely tendentiously; none of those sources are authoritative and you failed to cite any of the many in support of the present syntax and you also failed to acknowledge the allowance for the present syntax even in what you cited. It’s at the writer’s discretion. See, for example, [http://www.proofreadnow.com/blog/bid/57554/NONE-Is-it-singular-or-plural]. “Not one is visible to the naked eye.” Is there some reason you hate that? The right thing to do here is to change the sentence to something that isn’t going to cause this sort of dreary edit churn. [[User:Strebe|Strebe]] ([[User talk:Strebe|talk]]) 20:32, 28 September 2012 (UTC)
::I was not arguing that the use of "none is" is incorrect. I was arguing that the use of "none are" is just more fitting in this context. Maybe none of my sources were very authoritative but they all had a common consensus that "none are" is used with a plural, and I could find ten more. 
::The pair of sentences is: "However, due to their low luminosity, individual ''red dwarfs'' cannot easily be observed. From Earth, none is visible to the naked eye." In the first sentence, the plural "red dwarfs" is used, and the second sentence is directly connected to the first. This lead me to believe "none are" is more fitting here. It is not incorrect, but it lacked fluidity and never sounded right to me the moment I read it, and I was afraid it would bother other readers. But since I don't want to be debating such small details any longer, I will settle for the use of "not one" as a reasonable compromise even though it sounds too sharp to me. [[User:Cadiomals|Cadiomals]] ([[User talk:Cadiomals|talk]]) 21:37, 28 September 2012 (UTC)

:::By your reasoning, it would never be proper to write "none is" because the context is always a group. That’s what “none” does: It excludes the group. It never excludes the singular. The context you need to examine is the syntax within the sentence, not what’s going on in sentences around it. In the simplest case, “None is a friend,” vs. “None are friends.” English wants to distinguish between singular and plural, but it forgot about nongular (and it is equally awkward with collective nouns). To try to cope with that, we de facto transfer the subject to “friend” or “friends” and away from “none”. Strictly speaking, that shouldn’t be allowed, but that’s how English has evolved to (more or less) deal with its omission. In sentences like the one in question, there is no syntactical resolution; either way is equally reasonable and hence we are obliged to defer to the original writer. The “sounds wrong” argument doesn’t work. It sounds right to plenty of people. [[User:Strebe|Strebe]] ([[User talk:Strebe|talk]]) 01:38, 29 September 2012 (UTC)

== Reconciliation between minimum mass for self-sustaining fusion and red dwarf minimum? ==

In the article on STARS, it is stated that low metallicity protostars with a mass of 87 x Jupiter's is the lower bound for star formation.
Here, the lower bound is 0.075 x Sun's mass which is about a factor of 7 lower. I think this seeming discrepancy needs explanation.[[Special:Contributions/216.96.76.236|216.96.76.236]] ([[User talk:216.96.76.236|talk]]) 22:23, 20 June 2013 (UTC)

:Your "factor of 7" is the only discrepancy here. [[User:Strebe|Strebe]] ([[User talk:Strebe|talk]]) 09:32, 21 June 2013 (UTC)

== update ==

The section "planets" ought be updated after the discovery of Kepler 186f[[Special:Contributions/187.59.103.179|187.59.103.179]] ([[User talk:187.59.103.179|talk]]) 19:49, 19 April 2014 (UTC)

== External links modified ==

Hello fellow Wikipedians,

I have just added archive links to {{plural:1|one external link|1 external links}} on [[Red dwarf]]. Please take a moment to review [https://en.wikipedia.org/w/index.php?diff=prev&oldid=707242598 my edit]. If necessary, add {{tlx|cbignore}} after the link to keep me from modifying it. Alternatively, you can add {{tlx|nobots|deny{{=}}InternetArchiveBot}} to keep me off the page altogether. I made the following changes:
*Added archive http://web.archive.org/web/20070103234953/http://www.eso.org:80/outreach/press-rel/pr-2002/pr-22-02.html to http://www.eso.org/outreach/press-rel/pr-2002/pr-22-02.html

When you have finished reviewing my changes, please set the ''checked'' parameter below to '''true''' to let others know.

{{sourcecheck|checked=false}}

Cheers.—[[User:Cyberbot II|<sup style="color:green;font-family:Courier">cyberbot II</sup>]]<small><sub style="margin-left:-14.9ex;color:green;font-family:Comic Sans MS">[[User talk:Cyberbot II|<span style="color:green">Talk to my owner</span>]]:Online</sub></small> 18:19, 27 February 2016 (UTC)

== [[Draft:List of red dwarfs]] ==

There is a draft article called [[Draft:List of red dwarfs|List of red dwarfs]] that is nearly complete. Could some editors familiar with this topic check it over and possibly get it ready for mainspace? [[User_talk:Bradv|<span style="color:#C60">Brad</span>]][[Special:Contributions/Bradv|<span style="color:#C60">v</span>]] 00:30, 11 June 2018 (UTC)

== Definition ==

Every good article needs a definition.  This article has one, but it isn't universally loved.  Discuss.  [[User:Lithopsian|Lithopsian]] ([[User talk:Lithopsian|talk]]) 20:43, 5 June 2019 (UTC)

:That is not a definition, [[User:Lithopsian|Lithopsian]]. It is incoherent. Definitions are not incoherent. I fixed this, but you broke it again with [[WP:EDITWARRING]]. The current text:
:*States (A)
:::*''A '''red dwarf''' (or '''M dwarf''', '''M-type main-sequence star''', or '''red main-sequence star''') is a small and cool [[star]] on the [[main sequence]], of M [[spectral type]],''
::followed by (B),
:::''Red dwarfs range in mass from about 0.075 to about 0.50 solar mass and have a surface temperature of less than 4,000 K.''
::A and B contradict each other, since M dwarfs only reach 0.35 solar masses.
:*States, ''Sometimes [[K-type main-sequence star]]s, with masses between 0.50-0.8 [[solar mass]], are also included,'' 
::which ignores that K-type stars below 0.5 solar masses are (more likely to be) sometimes included.

:Now how about you stop exerting [[WP:OWNERSHIP]] and start explaining why your preferred text is better? Or else fix the problem instead of defending the incoherent status quo. [[User:Strebe|Strebe]] ([[User talk:Strebe|talk]]) 23:08, 5 June 2019 (UTC)

::My notes above are incorrect, since the 0.35 solar mass limit is for fully convective M dwarfs, not all, and K does not dip below 0.5 solar masses—at least, as far as the the sources I checked would commit to. I rewrote the lede in order to: (a) not define red dwarfs as synonymous with M dwarfs/M-type main-sequence star; (b) not dive into the definitional morass in the first paragraph and instead concentrate on traits that are true for any definition; (c) clearly state the lower bound of mass and temperature; (d) discuss the upper bounds in terms of the various definitions; (e) refer to the Definition section. Since red dwarf is not synonymous with M-type main-sequence star, the latter really ought to have its own page, just as [[K-type main-sequence star]] does. [[User:Strebe|Strebe]] ([[User talk:Strebe|talk]]) 02:00, 6 June 2019 (UTC)

== Minimal temperature ==
I am having trouble coming up with a rigorous source that is willing to commit to the least temperature a red dwarf could have. This seems to be partly because that number depends on chemical composition, and partly because it’s just really hard science, especially since late M dwarfs have a lot of dust production going on that helps obscure already faint signals. Several good papers explore the boundaries of red dwarf/brown dwarf transition as expressed by the LHS 1070 system (Köhler et al, 2012; Rajpurohit et al, 2012 for most recent), but they are unable to conclude whether LHS 1070B is a brown dwarf or a red dwarf. I infer by this that there isn’t much fusion going on in the lowest mass red dwarfs even though they are able to sustain it, and that therefore the transition is continuous between brown and red dwarf as far as measurable properties go—especially surface properties. That means the value is going to be known more from theory than from detection. Meanwhile the casual reader would probably like to have some number. I settled on ~2,500K on the basis of Köhler’s paper, but this would be for a Population I star, and I don’t find any numbers for Population II. I also perused endless lists of low mass stars, but (1) often they don’t state stellar vs brown dwarf; and (2) various sources often disagree considerably on the spectral type or surface temperature. Help? [[User:Strebe|Strebe]] ([[User talk:Strebe|talk]]) 04:51, 7 June 2019 (UTC)

: I am getting a clearer picture on why this isn't very clear. Surprisingly (to me) the most recent research thinks that the stellar cut-off is out of M entirely and near L2.0V (Dieterich et al, 2014: ''We find evidence for the local minimum in the radius-temperature and radius-luminosity trends that signals the end of the stellar main sequence and the start of the brown dwarf sequence at T eff ~ 2075 K, log (L/L ⊙) ~ -3.9, and (R/R ⊙) ~ 0.086. The existence of this local minimum is predicted by evolutionary models, but at temperatures ~400 K cooler[!].''), with mass yet to be determined. These results are still accepted in 2019 (Winters, Henry, Jao et al. 2019) and are very different than what our little article here discusses. Will update. [[User:Strebe|Strebe]] ([[User talk:Strebe|talk]]) 18:48, 7 June 2019 (UTC)

==“Artist's conception”==
I am not in favor of [https://en.wikipedia.org/w/index.php?title=Red_dwarf&diff=957065116&oldid=953316253 this change] in image. It’s hard to talk about “accuracy” in this context, given the impossibility of staring at the sun from a distance that would yield a comparable disc size, but in a relative sense, the new image doesn’t look significantly different from what a reader might expect of an image of our sun, other than the large sunspots. The previous image conveyed the comparatively dim nature of a red dwarf cogently. [[User:Strebe|Strebe]] ([[User talk:Strebe|talk]]) 07:20, 17 May 2020 (UTC)
:Agreed.  Policy is that artists' conceptions are generally only used from official sources.  Self-made images are considered [[WP:OR]].  I reverted the image, not just to the previous version which was itself a modification, but to the original which is direct from NASA.  [[User:Lithopsian|Lithopsian]] ([[User talk:Lithopsian|talk]]) 13:10, 17 May 2020 (UTC)
::That’s far too red even for the coolest red dwarfs (come on, NASA). I searched quite a bit for something suitable, but there is a curious lack of accessible sources. I think an effective portrayal would show the sun and a red dwarf (such as M9V) using similar simulated filtering and distance, but I can’t find any such thing. Maybe we should give up on an image. [[User:Strebe|Strebe]] ([[User talk:Strebe|talk]]) 18:14, 17 May 2020 (UTC)
:::That's presumably why the image was tweaked in the first place.  But then the replacement was just fanciful.  NASA press releases aren't the most scientifically precise.  [[User:Lithopsian|Lithopsian]] ([[User talk:Lithopsian|talk]]) 18:38, 17 May 2020 (UTC)
::::I put Red Dwarf Rendering.png back, providing references demonstrating that red dwarfs are orange in color and have starspots ([http://vendian.org/mncharity/dir3/starcolor/], [https://www.aanda.org/articles/aa/abs/2002/46/aa2017/aa2017.html]), and citing the last paragraph of [[WP:ASTROART]], which says "As with all guidelines, this guideline is not absolute and may be ignored according to common sense and discussion of individual cases. For example, a truly terrible artist's impression (sloppy artwork or blatant contradiction of known features) from a reliable source should not be included, nor should an excellent artist's impression (informative, minimal speculation, primarily depicting known features) be excluded because it is not from a reliable source." [[User:Lithopsian|Lithopsian]] reverted my edit twice, saying only to take it to the talk page. Well, here I am. If you want the article to have the NASA image (which does "blatantly contradict known features"), you need consensus to remove that paragraph from [[WP:ASTROART]]. [[User:SevenSpheresCelestia|SevenSpheresCelestia]] ([[User talk:SevenSpheresCelestia|talk]]) 20:50, 8 June 2020 (UTC)
:::::This has been discussed above. [[User:SevenSpheresCelestia|SevenSpheresCelestia]], why are you ignoring the objections that have already been listed? At least two editors here disagree that the image you reinstated is appropriate, for several reasons. You seem to be exercising [[WP:ownership]] of the article by repeatedly reverting, when you are instead obliged to obtain consensus for controversial edits. Let’s be more clear: The image you are trying to insert is [[WP:SYNTH]]. It cannot show correct black-body hue because it does not even contain a color profile, and even if it did, it would only be correct on somebody’s monitor calibrated in a particular way. Regardless, it’s not clear that that would be the best way to represent the color, given the impossibility of staring at a star with the naked eye from a distance implied by the image; given that color consists of more than hue; given that the dynamic range of an actual image exceeds the dynamic range of this synthesized image and therefore implies interpretation. The image may show large sunspots, which is fine, but what did it leave out? Where are the large-scale atmospheric dynamics? Given the large spectral range covered by the term “red dwarf”, which type is the portrayed one? The NASA image may not show the correct black body color for any spectral type, but given what most readers might use or think of as the sun’s color, for example, the ''relative'' color of the NASA image might be more informative, and I certainly believe the atmospheric dynamics represented in the NASA image are much more informative. The NASA image doesn’t answer some of the questions I raise, but, as a [[WP:RELIABLE]] source, it’s not obliged to whereas this new concoction is. In short, the image you promote is not suitable. Either there should be no image, or the article should use the NASA image. If a better image could be found as executed by an expert, then we should use that if it’s freely available. I haven’t found one. [[User:Strebe|Strebe]] ([[User talk:Strebe|talk]]) 03:54, 9 June 2020 (UTC)
::::::I'm not going to argue this further, but in any case the NASA image is highly inaccurate and, based on [[WP:ASTROART]] as it currently is, should not be in the article. [[User:SevenSpheresCelestia|SevenSpheresCelestia]] ([[User talk:SevenSpheresCelestia|talk]]) 17:59, 9 June 2020 (UTC)
:::::That's a somewhat selective reading of the guideline.  At least two people disagree that the unofficial image is "excellent" while the NASA one can hardly be called "truly terrible".  I would also prefer if you don't mis-characterise my edit comments; even if you didn't realise at the time, I was referring you to a discussion that had already taken place and that you were reversing without further discussion, then reversing again before going anywhere near the talk page.  They policy is [[WP:BRD|be bold, revert, discuss]], not be bold, edit war until you get your own way, then look at the talk page.  [[User:Lithopsian|Lithopsian]] ([[User talk:Lithopsian|talk]]) 20:41, 9 June 2020 (UTC)
::::::"blatant contradiction of known features" [http://vendian.org/mncharity/dir3/starcolor/] [https://www.aanda.org/articles/aa/abs/2002/46/aa2017/aa2017.html] :thinking:
::::::I've provided sources, can you? [[User:SevenSpheresCelestia|SevenSpheresCelestia]] ([[User talk:SevenSpheresCelestia|talk]]) 01:54, 10 June 2020 (UTC)
:::::::Which is exactly what makes it [[WP:SYNTHESIS]].  [[User:Lithopsian|Lithopsian]] ([[User talk:Lithopsian|talk]]) 13:58, 10 June 2020 (UTC)
== Reversion error ==
{{ping|Lithopsian}} [https://en.wikipedia.org/w/index.php?title=Red_dwarf&diff=1052450478&oldid=1052341345 this reversion] was some kind of slip on my part. Sorry about that. [[User:Strebe|Strebe]] ([[User talk:Strebe|talk]]) 00:46, 30 October 2021 (UTC)

==Why is there no Class G Stars article?==
There is an article for every other stellar class, except class G. Class G stars seem to instead be in the Red Dwarf article, even though not all red dwarfs are class G.  <!-- Template:Unsigned --><span class="autosigned" style="font-size:85%;">—&nbsp;Preceding [[Wikipedia:Signatures|unsigned]] comment added by [[User:Empika1|Empika1]] ([[User talk:Empika1#top|talk]] • [[Special:Contributions/Empika1|contribs]]) 00:29, 11 August 2022 (UTC)</span> <!--Autosigned by SineBot-->

{{small|Above undated message substituted from [[Template:Dashboard.wikiedu.org assignment]] by [[User:PrimeBOT|PrimeBOT]] ([[User talk:PrimeBOT|talk]]) 07:55, 17 January 2022 (UTC)}}

:You mean like [[G-type main-sequence star]]?  There is some inconsistency about which spectral types have a separate article and which don't, but there's also [[WP:GNG]] so possibly not everything should be in a separate article.  Is there something G-class-related that redirects here that you're concerned about?  [[User:Lithopsian|Lithopsian]] ([[User talk:Lithopsian|talk]]) 13:10, 11 August 2022 (UTC)

== Habitable planets far from a red dwarf? ==

If you had a mixture of potent greenhouse gases (CH2O, CO2, and CH4) and a thick atmosphere, you could have a planet further away from the star and yet habitable, right? These gases absorb a lot in the mid-IR regions (>3 microns wavelength) but are mostly transparent at near-IR and at wavelengths below 3 microns or so. The energy from the star would thus mostly pass through, while the planet's own blackbody emission would be mostly re-absorbed. [[Special:Contributions/209.104.252.130|209.104.252.130]] ([[User talk:209.104.252.130|talk]]) 17:19, 22 September 2022 (UTC)
: Please note that [[WP:NOTAFORUM|talk pages are not a discussion forum for the topic]]. [[User:Strebe|Strebe]] ([[User talk:Strebe|talk]]) 00:59, 23 September 2022 (UTC)