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 | |
| previous orbit statistics, both Galactic and stellar perturbations were taken into account | ||
|---|---|---|
| no. of returning VCs in the swarm | 5001 | * |
| no. of escaping VCs in the swarm | 0 | |
| no. of hyperbolas among escaping VCs in the swarm | 0 | |
| previous reciprocal semi-major axis [10-6 au-1] | 34.47 – 37.41 – 40.34 | |
| previous perihelion distance [au] | 363 – 412 – 451 | |
| previous aphelion distance [103 au] | 49.2 – 53.1 – 57.6 | |
| time interval to previous perihelion [Myr] | 4.16 – 4.62 – 5.17 | |
| percentage of VCs with qprev > 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).
| previous orbit statistics, here only the Galactic tide has been included | ||
|---|---|---|
| no. of returning VCs in the swarm | 5001 | * |
| no. of escaping VCs in the swarm | 0 | |
| no. of hyperbolas among escaping VCs in the swarm | 0 | |
| previous reciprocal semi-major axis [10-6 au-1] | 34.77 – 37.16 – 39.51 | |
| previous perihelion distance [au] | 12 – 15 – 19 | |
| previous aphelion distance [103 au] | 50.6 – 53.8 – 57.5 | |
| time interval to previous perihelion [Myr] | 4.01 – 4.4 – 4.85 | |
| percentage of VCs with qprev < 10 | 1 | |
| percentage of VCs with 10 < qprev < 20 | 94 | |
| percentage of VCs with qprev > 20 | 5 | |