Talk:(120348) 2004 TY364

"Other" TNO
What does Johnston mean with "Other TNO" exactly? --JorisvS (talk) 17:45, 13 November 2014 (UTC)


 * I assume he just means it does not easily fit into a single category of TNO. Classical and scattered both to seem to depend in-part on who is defining the term. Even some weak Resonant trans-Neptunian objects are not secure. -- Kheider (talk) 21:34, 13 November 2014 (UTC)
 * Right. In our case, we would simply list the different possibilities, of course, but it would not be so easy to do for Johnston's list, I'd say. What is Buie's definition for classicals? And are there other classifications in use that would place in yet another category (if not, listing Johnston would be pointless, and if so, we'd better list those)? --JorisvS (talk) 21:59, 13 November 2014 (UTC)
 * The Deep Ecliptic Survey (DES) found no clear boundary between the Classical and Scattered classes. I am not aware of another listing for TNO categories. The MPC likes to call just about everything with q>6AU a "Distant object" now-a-days. -- Kheider (talk) 22:42, 13 November 2014 (UTC)
 * Nice and vague of the MPC. Makes sense that there would not actually be any distinguishable boundary. Do I understand correctly from that paper that they only take cold classicals as "classicals" and all hot classicals as "scattered(–extended)"? --JorisvS (talk) 23:02, 13 November 2014 (UTC)
 * I know Buie moved the software to a new server a few years ago and I wonder if some gremlins are still in the software libraries. 90377 Sedna is coming up ScatNear and 20000 Varuna is coming up ScatExt. In other news, the MPC database calls centaur 52872 Okyrhoe (q=5.8) a main-belt object. -- Kheider (talk) 20:58, 16 November 2014 (UTC)
 * Well, that makes me wonder about other, unspotted mistakes in those. --JorisvS (talk) 12:32, 17 November 2014 (UTC)
 * This paper discusses the DES classification. They call objects Scat-Near if their time-averaged Tisserand parameter with respect to Neptune is less than 3. The current Tisserand parameter of Sedna, using their formula, is approximately 0.3, which explains why Buie has it as scattered-near. I don't know what this tells us about Sedna's orbit, though. The DES classicals have e>0.2 and TN>3. The latter can explain why high-inclination low-eccentricity KBOs may be classified as something other than classical. I can understand that inclination may have to be taken into account when identifying classicals, because otherwise scattered TNOs that had their orbits inclined by the Kozai mechanism, such as, may end up being considered classicals. The situation with Sedna makes me wonder if TN>3 is the best criterion, though. --JorisvS (talk) 14:10, 17 November 2014 (UTC)

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