C/2005 EL173 LONEOS
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C/2005 EL173 was discovered on 8 March 2005 by the LONEOS as an apparently asteroidal object in a retrograde orbit and semimajor axis of 36 au [MPEC 2005-F48, 2005 March 29]. Therefore it was initially classified as cubewano or scattered disc object in MPC. Its cometary apperance was reported by A. Fitzsimmons on 10 May 2005. C/2005 EL173 was observed until mid-November 2008.
This comet made its closest approach to the Earth on 4 January 2007 (3.310 au), two months before perihelion passage.
Solutions given here are based on data spanning over 3.7 yr in a range of heliocentric distances: 7.12 au – 3.886 au (perihelion) – 6.45 au.
NG orbit using full data-arc is determinable.
This Oort spike comet suffers rather slight planetary perturbations during its passage through the planetary system; however, these perturbations leas to escape this comet from the planetary zone on a hyperbolic orbit.
See also Królikowska and Dones 2023, Królikowska and Dybczyński 2017,and Królikowska 2014.
This comet made its closest approach to the Earth on 4 January 2007 (3.310 au), two months before perihelion passage.
Solutions given here are based on data spanning over 3.7 yr in a range of heliocentric distances: 7.12 au – 3.886 au (perihelion) – 6.45 au.
NG orbit using full data-arc is determinable.
This Oort spike comet suffers rather slight planetary perturbations during its passage through the planetary system; however, these perturbations leas to escape this comet from the planetary zone on a hyperbolic orbit.
See also Królikowska and Dones 2023, Królikowska and Dybczyński 2017,and Królikowska 2014.
| solution description | ||
|---|---|---|
| number of observations | 315 | |
| data interval | 2005 03 03 – 2008 11 17 | |
| data type | perihelion within the observation arc (FULL) | |
| data arc selection | entire data set (STD) | |
| range of heliocentric distances | 7.12 au – 3.89 au (perihelion) – 6.45 au | |
| type of model of motion | NC - non-gravitational orbits for symmetric CO-g(r)-like function | |
| data weighting | YES | |
| number of residuals | 627 | |
| RMS [arcseconds] | 0.41 | |
| orbit quality class | 1a | |
| next orbit statistics, both Galactic and stellar perturbations were taken into account | ||
|---|---|---|
| no. of returning VCs in the swarm | 0 | |
| no. of escaping VCs in the swarm | 5001 | |
| no. of hyperbolas among escaping VCs in the swarm | 5001 | * |
| next reciprocal semi-major axis [10-6 au-1] | -18.86 – -16.20 – -13.40 | |
| next perihelion distance [au] | 117 – 122 – 127 | |
| synchronous stop epoch [Myr] | 2.35 | S |
| percentage of VCs with qnext > 20 | 100 | |
Upper panel: Time distribution of positional observations with corresponding heliocentric (red curve) and geocentric (green curve) distance at which they were taken. The horizontal dotted line shows the perihelion distance for a given comet whereas vertical dotted line — the moment of perihelion passage.
Middle panel(s): O-C diagram for a given solution (sometimes in comparison to another solution available in CODE), where residuals in right ascension are shown using magenta dots and in declination by blue open circles.
Lowest panel: Relative weights for a given data set(s).
Middle panel(s): O-C diagram for a given solution (sometimes in comparison to another solution available in CODE), where residuals in right ascension are shown using magenta dots and in declination by blue open circles.
Lowest panel: Relative weights for a given data set(s).
| next orbit statistics, here only the Galactic tide has been included | ||
|---|---|---|
| no. of returning VCs in the swarm | 0 | |
| no. of escaping VCs in the swarm | 5001 | |
| no. of hyperbolas among escaping VCs in the swarm | 5001 | * |
| next reciprocal semi-major axis [10-6 au-1] | -18.76 – -16.11 – -13.32 | |
| next perihelion distance [au] | 3.39 – 3.76 – 4.14 | |
| synchronous stop epoch [Myr] | 2.46 | S |
| percentage of VCs with qnext < 10 | 100 | |