Talk:List of largest exoplanets

Ranking

The ranking makes no sense, the ranks listed here only concern the entries list here, and not the ranking of all known planets. Therefore I am removing ranking -- 67.70.35.44 (talk) 07:59, 7 November 2014 (UTC)

HD 100546 b

This radius is almost certainly wrong; the object seems to be surrounded by a protoplanetary disk. I cannot find any original source for this radius in the papers. There's no way it has a radius more than 6x that of Jupiter. This may be a typo of its semi-major axis. Removing pending someone finding a better source. Titanium Dragon (talk) 00:57, 26 February 2017 (UTC)

There is a rediable source which mentions the radius of HD 100546 (6.9 R_J). see: Confirmation and characterization of the protoplanet HD100546 b - Direct evidence for gas giant planet formation at 50 au. Ynoss ^(talk) 18:45, 22 May 2017 (UTC)

Actually, HD 100546 b might actually be a brown dwarf. According to planetary evolution and physics models, there is no planet with a diameter of 350,000 km or more. Thus ROXs 42 Bb, GQ Lupi b and HD 100546 b might actually be brown dwarfs. Thus it would be improper to say that they are the biggest planets, and CT Cha b (316 000 km) will get the record for now. --Joey P. - THE OFFICIAL (talk) 03:35, 14 July 2017 (UTC)

No. HD 100546 b, ROXs 42Bb and GQ Lupi b are planets because they are not massive enough. To be brown dwarfs, they must have a mass greater than 30 solar mass.Thank you— Ynoss du 44 Pro ★ ✉ / _CONTRIBS 05:58, 14 July 2017 (UTC)

im going to add hd 100546 b into this so people can think the radius is right 2600:1700:82B0:7480:3D45:583F:9438:96B7 (talk) 00:43, 18 August 2023 (UTC)

GQ Lup b

In the paper sourcing its radius, this "planet" is estimated as having a mass of ~20 M_J, which would make it a brown dwarf, not a planet, and the paper notes that it is probably a brown dwarf but that they cannot rule out that it might be smaller. Removing it for now; feel free to argue with me if you've got a good reason why this should be here. Titanium Dragon (talk) 01:15, 26 February 2017 (UTC)

List of most massive exoplanets say that the most massive exoplanet is DENIS-P J082303.1-491201 b with a mass 28.5 M_J so the maximum mass of a planet is 30 M_J. Ynoss ^(talk) 18:55, 22 May 2017 (UTC)

Radii

Please reconsider the given radii. An old planet cannot have a radius of 3 - 4 times Jupiter's. Please see http://beyondearthlyskies.blogspot.fr/2015/07/classifying-planets-brown-dwarfs-stars.html figure 3. There is a reason why e.g. for HD 87883 b neither exoplanet.eu http://exoplanet.eu/catalog/hd_87883_b/ nor NASA exoplanet archive https://exoplanetarchive.ipac.caltech.edu/cgi-bin/DisplayOverview/nph-DisplayOverview?objname=HD+87883+b&type=CONFIRMED_PLANET give a radius, since RV planets only have a radius determined if a transit is observed, which I assume is not the case here. Directly imaged planets can have a radius, coming from luminosity / age / temperature. Very young planets still contract, thus are larger. — Preceding unsigned comment added by Exowrite (talk • contribs) 13:23, 23 November 2017 (UTC)

@Exowrite: I think this source http://www.exoplanetkyoto.org/exohtml/A_All_Exoplanets.html is somewhere unreliable. Well, what I will do is remove all the planets mentioned in this source and add more planets that have radii larger than 1.7 R_J. ZaperaWiki44^{(✉/Contribs)} 08:33, 25 January 2018 (UTC)

Pictures, or no Pictures ?

I see that a particular IP address user does not want to have pictures in this list.

I see no reason for those planets not to be there.

1.) They aren't hurting anyone, and they aren't doing anything wrong staying there, are they?

And 2.) So what if it's a list, nobody said that pictures can't stay on a list. There is no law preventing pictures staying there. As far as I can see, you are just removing them because you don't like them.

Please clarify,

PNSMurthy (talk) 01:18, 20 July 2020 (UTC)

I want those images to Stay . I am undoing the edit. The descriptions likely stand no justice to the image. For HD 100546b, It says there is a disk around the planet, and the image shows that. --THE COLOSSAL GALAXY NAMED IC1101 (talk) 11:29, 21 July 2020 (UTC)

Indeed. There's no reason for them to go, so, why don't they stay?PNSMurthy (talk) 00:24, 23 July 2020 (UTC)

They SHOULD Stay. Scientific data and real pictures of exoplanets are basically a bit of blobby like appearance. Kind of ugly , right? So we want a better image, and that’s where the artist images are here for. Again, HD 100546b for example, The real image when you look at it you can’t see the planet and disk but using the artist’s impression, we can visualize an impression of the planet and disk. Also see the red orange and yellow color of HD 100546b means it is hot. Using Artist images, At least we are able to visualize a guess of how the planets look like. THE COLOSSAL GALAXY NAMED IC1101 (talk) 03:46, 23 July 2020 (UTC)

The problem is that they don't have really much use for the list and many are already used respectively in exoplanets' linked articles, despite replies here since there is no really much proper explanation. Some instead just show also the location of the objects within a planetary system, in which it feel as well useless for the list too. And what is even worse (aside from impressions just made-up by users as for WASP-76b), few used in the list are just a comparison with Jupiter by radius while using the exoplanet as the white sphere.

Speaking of HD 100546 b, it was honestly more reasonable to just remove it from the list (and it is already), the quoted radius was never meant to a single planatary radius but instead of the emitting area anyways. NASA Exoplanet Archive also is not as reliable as scientific papers (and also never stated HD 100546 b as the "largest exoplanet" despite being at the top of the list by radius), and has some strange and nonsensical results that are likely made-up, such as 752 M_J when one of the most recent researches placed a much lower upper limit of 1.65 M_J. Moreover the surrounding disk is also much larger with a radius up to 0.44 AU based on the same said study. Regards—ZaperaWiki44^{(✉/Contribs)} 01:18, 7 October 2023 (UTC)

A Commons file used on this page or its Wikidata item has been nominated for deletion

The following Wikimedia Commons file used on this page or its Wikidata item has been nominated for deletion:

• Kepler-39 b.jpg

Participate in the deletion discussion at the nomination page. —Community Tech bot (talk) 17:09, 31 March 2021 (UTC)

Tell

Largest planet 223.235.189.226 (talk) 03:14, 29 March 2022 (UTC)

Remove HD 100546 b

This is the radius of the emitting area, not the radius of the actual planet and this is explicity mentioned in the source. Faren29 (talk) 16:03, 12 June 2022 (UTC)

HOW COME 2600:1700:82B0:7480:3D45:583F:9438:96B7 (talk) 00:41, 18 August 2023 (UTC)

HD 100546 b disputed

New analysis showed that signals from what appeared to be HD 100546 b were from a more diffuse structure.

The visible part of the source may not have been part of such planet itself, but the disturbance in disk caused by what appears to be a much smaller and further body (c) completely embedded in the dust shroud.

The 3rd candidate is not confirmed and seems obvious from the recent analysis of the previous disputations.[1] Eric Nelson27 (talk) 21:03, 11 June 2023 (UTC)

TYC 8998-760-1 b's status

TY 8998-760-1 is around 14 x the mass of Jupiter, with a margin of error of +/- 3 Jupiter masses, meaning there's a high chance it's a brown dwarf rather than a true planet.

To call it a planet may not always be truthful because the average mass is 14 Jupiters and it takes at least 13 Jupiters in mass for it to qualify as a brown dwarf.

TYC 8998-760-1 b is most likely a brown dwarf due to its mass. Eric Nelson27 (talk) 21:40, 16 June 2023 (UTC)

Rewriting the list

Hello. I wanted to let you know that I have made a workpage (or sandbox) to rewrite the list in order to make it better organized given this list is an overall mess.

See also the #Pictures, or no Pictures ? subject regarding the files used in the table, and why I disgreed from the beginning. Regards—ZaperaWiki44^{(✉/Contribs)} 16:41, 4 October 2023 (UTC)

RIK 72 b

i found this source [1901.05532] Age Determination in Upper Scorpius with Eclipsing Binaries (arxiv.org) saying RIK 72 b is around 3.10 Rj, is this reliable? ADudeWhoLikesAstronomy65141 (talk) 10:43, 29 January 2024 (UTC)

This source is likely reliable, however, this object could not be on the list because its mass (59.2±6.8 M_J) makes it obviously a brown dwarf. InTheAstronomy32 (talk) 16:31, 29 January 2024 (UTC)

Disputed bodies vs candidate bodies

The body HD 100546 b was added to the page again, and since it's disputed, I had to correct the page.

There are 2 candidate bodies, but none of them are named b, c, or d, and they have no radii estimated (yet they're not confirmed nor disputed at the time of this topic).

b, c, and d on the other hand are disputed.

Therefore, there are no known planetary-sized or substellar bodies orbiting HD 100546.

Anyone on here should be reminded not to add disputed objects on the page because that's evidence they don't exist. Eric Nelson27 (talk) 19:00, 2 April 2024 (UTC)

UScoCTIO 55

The object is also rogue like proplyd 133-353 and it is estimated around 4.9 Jupiter Radius with a mass of 10 Jupiter mass, sould we add it to the list? APerosn53248 (talk) 13:34, 20 July 2024 (UTC)

0.10 M_☉ according to this paper SpaceImplorerExplorerImplorer 20:15, 21 July 2024 (UTC)

A New List

Sould we do instead of 1 list, 2 lists?, one being for exoplanets and one being for brown dwarfs/sub brown dwarfs? APerosn53248 (talk) 09:48, 30 July 2024 (UTC)

ROXs 42Bb

If we are using the best and most recent estimates (see caevats section), then ROXs 42 Bb should be at 2.83±0.01 R_J. 21 Andromedae (talk) 12:15, 4 August 2024 (UTC)

1.35 R_J should also be replaced with something more sensible such as 1.81 R_J, that uses the mass and surface gravity from the high-resolution retrievals. Actually i support putting the radius at 2.83 R_J, it is the most recent estimate anyway and is consistent with evolutionary models. 21 Andromedae (talk) 12:27, 4 August 2024 (UTC)

Removing HD 100546 b

there is no reason to add disputed bodies to the list if we know they don't exist so im removing it from now 2A00:A041:E547:500:78DB:3F9E:1B51:F418 (talk) 12:40, 7 August 2024 (UTC)

Sub-brown dwarfs vs. Rogue planets (PSO J318.5−22)

I first also wanted to write that we don't have a time machine, thus not knowing how PSO J318.5-22 formed. So both Sub-brown dwarf and Rogue planet should be linked. However, I realized a problem wiith the definition of both types of objects. In Sub-brown dwarf Rogue planets are defined as 'rogue planets, which originally formed around a star and were ejected from orbit', while in Rogue planets the objects are defined independent of the formation like a star or a planet. Having read the first type of definition, I assumed we don't know whether the object was ejected, so PSO J318.5−22 could be a sub-brown dwarf or a rogue planet. Vice versa, there is a similar problem with the definitions: In Rogue planets Sub-brown dwarfs are defined as 'Some planetary-mass objects may have formed in a similar way to stars, and the International Astronomical Union has proposed that such objects be called sub-brown dwarfs.', which is incorrect. In Sub-brown dwarfs they are defined as ''the IAU Working Group on Extra-Solar Planets (WGESP), which defined it as a free-floating body found in young star clusters below the lower mass cut-off of brown dwarfs.'

The problem can be solved consulting the most recent working definition of exoplanet. Either at [2] or at the Exoplanet page. In the 'List of possible sub-brown dwarfs' at Sub-brown dwarfs several objects are given 'orbiting one or more stars'. However, according to definition objects below 13 Jupiter masses 'that orbit stars or stellar remnants are "planets" (no matter how they formed).' So, either planets or brown dwarfs (if above the limit), never sub-brown dwarfs.

Similarly, '

• Free-floating objects in young star clusters with masses below the limiting mass for thermonuclear fusion of deuterium are not "planets", but are "sub-brown dwarfs" (or whatever name is most appropriate).

' So, also independent of formation. If an object is formed around a star like a planet and ejected, it is according to this definition a sub-brown dwarf. Also if it was formed like a star, ejected from a system or not.

This leads to the fact that 'Sub-brown dwarfs and rogue planets are not essentially the same thing'. This is corraborated twice in [3]. Once in section 4 'Future': ' At the end of item (3), the text: “sub-brown dwarfs” (or whatever name is most appropriate) should be updated to the currently accepted term “free-floating planetary mass objects”.' And even more clear in section 2.6.: 'For planetary mass objects that do not orbit around a more massive central object, the term “sub-brown dwarf” has not been adopted in the usage by the community; rather, these objects are often referred to as “free floating planetary mass objects”. These two terms are nowadays considered as synonymous'.

So, I strongly suggest to merge the two pages Sub-brown dwarf and Rogue planet. While it seems more work was invested into the latter page, a level-5 vital article below 'exoplanet' might be problematic, as is currently the case for the latter page, since '

• Free-floating objects in young star clusters with masses below the limiting mass for thermonuclear fusion of deuterium are not "planets"

'

This leads to follow-up difficulties, e.g. none of the objects in the List of directly imaged exoplanets can be a Sub-brown dwarf, since not free-floating, they are either planets or brown dwarfs, except the excluded free-floating planetary mass objects / free-floating planets / sub-brown dwarfs / rogue planets / ... . Stevinger (talk) 11:57, 8 August 2024 (UTC)

It seems surprisingly hard to find references for the original usage of 'sub-brown dwarf' (which confirms 'the term “sub-brown dwarf” has not been adopted in the usage by the community'[4]) and also to an extent 'rogue planet'. This explains the partly inconsistent definitions on the dedicated pages and a small amount of references therein.

The following two references could be added: 'One doesn't know if apparently "free-floating" planets which may have recently been discovered in Orion formed by self-collapse or by formation in a disk followed by ejection (Reipurth 2003)'[5] and: 'if it turns out that Jupiter has no real core and formed suddenly during a rapid gravitational instability in the protoplanetary nebula, that we have been mistaking a sub-brown dwarf for a planet all this time'[6]

The latter reference confirms that 'sub-brown dwarf' was used for objects formed like stars, also within a system, contradicting the current IAU working definition of exoplanet.[7] In this definition all objects below 13 Jupiter masses 'that orbit stars or stellar remnants are "planets" (no matter how they formed).' and 'free-floating objects in young star clusters with masses below the limiting mass for thermonuclear fusion of deuterium are not "planets", but are "sub-brown dwarfs" ' It also explains why the IAU working group explicitly wrote 'nowadays' in 'These two terms (sub-brown dwarf and rogue planet) are nowadays considered as synonymous'.

Should the definitions of the two terms be updated with additional references for the traditional meaning of the terms OR should the two articles be merged taking into account the IAU working definition of exoplanet and the two terms NOWADAYS considered as synonymous? Stevinger (talk) 05:28, 9 August 2024 (UTC)

Help

Im adding objects to the list but i thought the references mention the size and the mass, but i did put the link in and it putted a different reference 77.137.65.183 (talk) 20:04, 9 August 2024 (UTC)

That is weird, should not happen. If you post a link in the discussion, here, as reply someone can surely put it into the list. Stevinger (talk) 02:31, 10 August 2024 (UTC)

Proplyd 133-353

In this edit user 21.Andromedae states Re-added Proplyd 133-353, calculating a radius from temperature and luminosity is not wp:SYNTH (not anything else) per this discussion. Even if this kind of calculation is acceptable, there are two points to be made here:

• The footnote merely says Based on the estimated temperature and luminosity, it does not say how the values were calculated. So it is not reproducible.
• Proplyd 133-353 is a proplyd. Does its disk affect the values used here?

SevenSpheres (talk) 20:06, 10 August 2024 (UTC)

The footnote can be improved with the footnote used in Epsilon Indi Ab. 21 Andromedae (talk) 20:51, 10 August 2024 (UTC)

Multiple issues

Following a recent series of edits, I believe there are multiple issues with this list that need to be addressed.

1. The usage of artists' depictions for exoplanets in this list is unusual and, in my opinion, unwarranted. There was indeed an earlier discussion about this topic, but this discussion only had three participants—two of whom failed to make any reasonable justification as to why such images should be kept. This cannot reasonably be regarded as consensus in favor of keeping these illustrations. Though WP:ASTROART hasn't any specific guidelines for lists, I believe this excerpt applies: When choosing images to illustrate astronomical objects, editors should select images with maximum potential to inform readers and minimum potential to misinform readers. At best, these illustrations serve no meaningful, much less encyclopedic purpose—this is a list about exoplanet sizes, after all. At worst, several of these illustrations are blatantly misinformative: the TrES-2b illustration depicts exomoons where none have been confirmed. This is an issue that is only exacerbated seeing as actual imagery is thrown into the mix.
2. Related to the issue regarding Proplyd 133-353, many of the entries in this list are extremely young (< 20 Myr) objects surrounded by dust and gas, including GJ Lup b, OTS 44, and DH Tauri. These objects are surrounded by large amounts of gas and dust that significantly affect their thermal emission, therefore also affecting any size estimate for these objects and making them appear larger than feasibly possible. This, at the very least, requires a big caveat on this influence, if not excluding these objects entirely.
3. Several entries are also accompanied by additional information. Most simply include mass and other basic information, but several that I had removed before they were reinstated contain significant amounts of trivial information. Major sourcing/prose issues aside, what warrants the inclusion of material such as the ambiguous a very puffy hot Jupiter, The tidally-locked planet where winds move 18,000 km/h, and where molten iron rains from the sky due to daytime temperatures exceeding 2,400 °C (4,350 °F), or This planet is so close to its parent star that its tidal forces are distorting it into an egg-like shape.? I understand including information for planets that represent significant milestones or have additional exceptional properties, but beyond those this feels uncomfortably close to MOS:MISC.

ArkHyena (talk) 20:21, 10 August 2024 (UTC)

@21.Andromedae, Stevinger, APerosn53248, and Foxy Husky: You were all actively editing the list at the same time during August 2024. Would you all mind to explain and address these concerns? Nrco0e (talk • contribs) 20:24, 10 August 2024 (UTC)

To clarify ArkHyena's point about surrounding dust around young objects, I'd like to mention that HD 100546 b suffers the same problem as GQ Lup b, DH Tau b, etc. with surrounding dust making them appear brighter than they really are. I don't see a reason why just HD 100546 b is excluded from the list, but not those objects. Nrco0e (talk • contribs) 20:31, 10 August 2024 (UTC)

Also pinging @SpaceImplorerExplorerImplorer since you have extensive involvement with superlative lists. What are your thoughts on these concerns? Superlative lists like this tend to be highly popular to the general public, so quality control is important. I believe that including appropriate caveats like surrounding dust is equally as important as having accurate size estimates in this list here. Nrco0e (talk • contribs) 20:53, 10 August 2024 (UTC)

The existence of HD 100546 b is disputed. 21 Andromedae (talk) 21:18, 10 August 2024 (UTC)

Strongly support removing the image column from this and other lists, but the main editors of these lists are going to disagree. SevenSpheres (talk) 20:25, 10 August 2024 (UTC)

I strongly oppose the removal of artistic illustrations, they are interesting, useful, illustrate the article and, contrary to what has been said, they are informative in nature. Take WASP-12b as an example, the text says that "This planet is so close to its parent star that its tidal forces are distorting it into an egg-like shape. As of September 2017, it has been described as "black as asphalt", and as a "pitch black" hot Jupiter as it absorbs 94% of the starlight that reaches its surface." and the artistical illustration show this. This list will probably be seen by laypeople and the illustrations make the these large planets better understood. 21 Andromedae (talk) 21:12, 10 August 2024 (UTC)

That information is irrelevant to the planet's size and belongs in the article on the planet itself. Please also consider the fact that artist impressions do not necessarily "make planets better understood"; they can also misinform readers, for example by giving the false impression that a hot Jupiter would appear pitch black to the eye, or that we know more about a planet's size and composition than we really do. SevenSpheres (talk) 21:25, 10 August 2024 (UTC)

If an artistic illustration is misleading, remove it. It is a list of the largest exoplanets, but may also contain additional information. The list of nearest stars, for example, contains information about the constellations, masses, coordinates, and so on, of the nearest stars, even when these things are loosely related to the list's scope. 21 Andromedae (talk) 22:05, 10 August 2024 (UTC)

@21.Andromedae: Forgive me for being overly pedantic and playing devil's advocate here, but would WASP-12b really appear "pitch black" when it's so close to its star?

At its distance from its star, WASP-12b receives 1.04×10⁷ W/m² ≈ I = L_star/4πa_orbit² of starlight, using WASP-12b's orbital radius and star luminosity from their Wikipedia infoboxes. Given WASP-12b's radius, it receives 6.04×10²³ W = I·A_WASP12b of starlight on its star-facing hemisphere (assume a circular surface area A_WASP12b = πR_WASP12b² for WASP-12b's single hemisphere, due to it being tidally locked). Since WASP-12b reflects 8.6% of the total light it receives (from the latest geometric albedo measurement in 2024, which isn't in the Wikipedia page), multiplying the planet's geometric albedo with the starlight received in Watts tells us that WASP-12b is reflecting approximately 5.19×10²² W of light from its star-facing hemisphere. The total reflected starlight from WASP-12b is almost 29 million times brighter (in Watts) than Earth's Moon, which reflects 1.81×10¹⁵ W of the Sun's light and appears bright to us on Earth! (for a solar irradiance of 1361 W/m², aka the solar constant, and Moon geometric albedo of 0.14). Furthermore, WASP-12b has an equilibrium temperature of 3000 K (from the latest paper on this), which is hot enough that it would visibly glow red over its entire surface. Assuming WASP-12b is a blackbody with emissivity of 0.9, it would emit roughly 680000 W/m² of 700 nm (red) light, corresponding to a luminosity of 1.6×10²³ W when multiplied by WASP-12b's spherical surface area. The thermal emission luminosity is roughly 4.1 times higher than the amount of starlight WASP-12b reflects! (Blackbody calculations here)

Therefore, the pop media claim of "pitch black" hot Jupiters is nothing more that a terrible misunderstanding of albedo vs. flux/light intensity. This is why I personally am skeptical of pop media portrayals of planets and other astronomical bodies. Nrco0e (talk • contribs) 23:27, 10 August 2024 (UTC)

If you want a more accurate illustration of WASP-12b, this image is the way to go. File:WASP-12b a Hot, Carbon-Rich Planet.jpg Nrco0e (talk • contribs) 23:27, 10 August 2024 (UTC)