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Including Sedna in the Oort cloud is speculation and should not be enshrined as accepted classification. kwami 02:40, 2005 August 2 (UTC)
Since when is Triton trans-Neptunian? Ken Arromdee 15:46, 23 September 2005 (UTC)
I created an article for (55637) 2002 UX25, it's just a stub for now. I couldn't find any more information, but it has the orbital elements. shaggy 01:22, 20 December 2005 (UTC)
Not to be overposessive of a template I created or anything, but I think a simple KB/SD bifurcation makes more sense in the template. For one, we don't have to mix multiple levels of taxon—spatial-region-a and spatial-region-b is a simple divide, while spatial-region-a-objects, spatial-region-b-objects-with-orbital-characteristics-x and spatial-region-b-objects-with-orbital-characteristics-y is needlessly muddled. Secondly, the KB/SD split preserves the convention of going innermost to outermost, as no KBO is closer to the sun than any SDO (short-term orbital overlaps aside), while cubewanos and plutinos have a hopelessly intermingled neighborhood with no one set clearly closer or farther from the sun (plutinos are, on average, closer, for what it's worth). Finally, there are no shortage of orbital-characteristic-based categorizations that could be applied, despite the fact the template gives the impression there are only three. SDOs, for instance, can be subdivided between those in resonant and non-resonant orbits (2003 UB313 being in 17:5 or something bizarre like that), while KBOs have been found in all manner of odd resonances other than just 3:2 (plutino) and nonresonant (cubewano). -The Tom 15:54, 2 October 2005 (UTC)
There's an interesting alternate list here. By their estimation 2002 UX25 should be off and 1996 TL66 and Huya should be on. --Patteroast 23:57, 9 July 2007 (UTC)
I want to move this template to "Template:Plutoids" because it is more concise. In addition, I do not understand why User:Ckatz revert my move... UU (talk) 08:53, 13 May 2009 (UTC)
Combined the two KB sections and the two SD sections. Also changed the wording "candidates" to "likely": they either are DPs or they are not. They are not candidates that will become DPs if recognized. — kwami (talk) 20:44, 23 December 2012 (UTC)
As Ruslik0 said in his edit summary, "no reason to single out these three bodies". (Though there is consensus that the IAU five should be separated to some extent.) — kwami (talk) 22:15, 25 December 2012 (UTC)
Okay, I think that's acceptable. It's weird to call them "candidates", since it's not like they become DPs after being evaluated, but that's the wording we use in other articles, so if we change it we should change it everywhere. — kwami (talk) 19:58, 26 December 2012 (UTC)
We now have Vesta as a possible former DP. Actually, it's quite clear that it once as a DP, so I don't think we need the question mark. That would be better suited to Psyche and Eunomia, both of which show evidence of differentiation. If we're going to add Vesta, shouldn't we add all known or suspected former DPs in the asteroid belt? What about Phoebe? Triton? — kwami (talk) 20:43, 9 March 2015 (UTC)
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Gotta go, but I don't think "disrupted out of equilibrium" is right. They froze out of equilibrium and because of that couldn't recover from subsequent battering.
Also, the list (not your version) is getting ridiculous. The list of "possible" DPs (as in anything that could possibly be 200 km in diameter) would be pages long. — kwami (talk) 23:54, 28 August 2015 (UTC)
All either have an ellipsoidal shape (Pallas, Eunomia, Psyche) or an unknown shape (Hygiea) and are also above 200km. They are the only ones that meet both criteria, hence why I seeked to include them. Changing it to "frozen out of equilibrium" would be a good change. DN-boards1 (talk) 00:03, 29 August 2015 (UTC)
http://astro.troja.mff.cuni.cz/projects/asteroids3D/data/archive/1-1000/A483.M783.shape.png
Not QUITE round, possibly a former DP?
But Pallas....
http://astro.troja.mff.cuni.cz/projects/asteroids3D/data/archive/1-1000/A101.M101.shape.png
http://astro.troja.mff.cuni.cz/projects/asteroids3D/data/archive/1-1000/A101.M102.shape.png
I uhh...see a slightly irregular sphere. A prolate spheroid. The lightcurve models seem to show HE in Pallas but not Cybele, Hygiea, Psyche, etc. Pallas is quite clearly close to or in HE. We had some data, i.e. the HST images, that left some questions, but now we have lightcurve data. This obviously looks round. In fact, thus far, it's the ONLY one besides Ceres to do this, to be almost perfectly round. I mean seriously, look at the images. Am I the only one who sees an object in HE here? DN-boards1 (talk) 21:42, 2 October 2015 (UTC)
I'm concerned about the development of some of these lists, like that represented by this template on dwarf planets. Wikipedia is supposed to rely on sources. It is not supposed to rely on original research. Yes, it might sometimes seem clear to an individual editor that this or that small chuck of stuff is or is not a dwarf planet, or, similarly, whether it is or is not in hydrostatic equilibrium. But in other cases it really is not clear and it is not for us to try to label things without a source. I perceive that there is some inference going on in the case of this template on dwarf planets. In particular, we have listed as "see also" Charon, Vanth, Dysnomia, and Hi'iaka. Other objects are listed as well. Why? Are these recognized as "dwarf planets" as per some cited source? Yes or no? Is this just some vague association that is being suggested because these are objects that happen to orbit officially designated dwarf planets? The uninitiated reader of the template is not given a clue. What about the objects put into the various categories in this template? Are each of these reliably sourced? More generally, we should not feel compelled to fill out lists of objects, putting this or that object into one or more of several different categories. Lists don't need to be complete. Reporting that an object belongs in a certain category should not rely on our own original research. It should only rely on a cited source. Isambard Kingdom (talk) 06:40, 19 September 2015 (UTC)
-The organization into plutinos, etc. is for convenience. The Kuiper belt section was getting overly long and crowded, so it was divided into more accurate categories, per the DES. -Charon, Vanth, Dysnomia, and Hi'iaka have sometimes been called "binary dwarf planets" as A) They are in hydrostatic equilibrium B) They are of a large size compared to their parent body - the ratio is actually quite amazing, considering the size. They each cause a noticeable effect on their parent dwarf planet (I'll consider Orcus to be a DP for convenience here), in the case of Charon and Vanth causing them and their parent body to revolve around a barycenter outside either body, and in the case of Dysnomia and Hi'iaka being prominent and causing them and their parent bodies to be tidally locked to one another.
Basically, those four, if the IAU allowed binary dwarf planets, WOULD be considered DPs. --DN-boards1 (talk) 05:16, 20 September 2015 (UTC)
Just noting that the black and white photo of Ceres should be replaced with the colour version released in October. 134340Goat (talk) 04:14, 4 March 2016 (UTC)