EDP Sciences
Free Access
Issue
A&A
Volume 547, November 2012
Article Number L2
Number of page(s) 7
Section Letters
DOI https://doi.org/10.1051/0004-6361/201220377
Published online 31 October 2012

Online material

Table 2

Heliocentric Keplerian orbital elements of Neptune’s L4 Trojans (I): 2001 QR322, 2004 UP10, and 2005 TN53.

Table 3

Heliocentric Keplerian orbital elements of Neptune’s L4 Trojans (II): 2005 TO74, 2006 RJ103, and 2007 VL305.

Table 4

Heliocentric Keplerian orbital elements of Neptune’s L5 Trojans: 2004 KV18, 2008 LC18, and 2011 HM102.

thumbnail Fig. 4

Evolution of various parameters during the time interval (–500, 500) kyr for three Neptune L4 Trojans: 2001 QR322, 2004 UP10, and 2005 TN53. The distance to the objects from Neptune is given in panel A); the value of the Hill sphere radius of Neptune, 0.769 AU, is displayed. The resonant angle, λr, is displayed in panel B) for the nominal orbit (source: JPL Small-Body Database and AstDyS-2). The orbital elements are depicted in panel C), a with the current value of Neptune’s semi-major axis, panel D), e, and panel E), i. 2005 TN53 appears to be the most stable of Neptune’s Trojans and 2001 QR322 the one with the largest libration amplitude.

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thumbnail Fig. 5

Same as Fig. 4 but for Neptune L4 Trojans: 2005 TO74, 2006 RJ103, and 2007 VL305. 2007 VL305 exhibits the second largest libration amplitude among L4 Trojans.

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thumbnail Fig. 6

Same as Figs. 4 and 5 but for Neptune L5 Trojans: 2004 KV18, 2008 LC18, and 2011 HM102. The dynamical evolution of 2004 KV18 is clearly different and it is the most unstable of the “classical” Neptune Trojans. The most recent discovery, 2011 HM102, is the most stable L5 Trojan and it may be as stable as 2005 TN53, likely the most stable of Neptune’s Trojans.

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© ESO, 2012

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