C/2014 AA52 Catalina
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Comet C/2014 AA52 was discovered on 11 January 2014 by R.A. Kowalski during Catalina Sky Survey, that is about a year and two months before its perihelion passage, and was followed until 20 September 2015. This comet had closest approach to the Earth on 24 December 2014 (2.08 au, almost two months before the perihelion passage).
This is a comet with NG effects manifested in positional data fitting. Solutions 'a5' (GR) and 'n5' (NG, preferred) are based on data spanning over 1.7 yr in a range of heliocentric distances: 4.93 au – 2.00 au (perihelion) – 3.11 au.
This Oort spike comet suffers tiny planetary perturbations while passing through the planetary system; these perturbations lead to a slightly more tight future orbit, still inside the Oort Cloud (see future barycentric orbits).
This is a comet with NG effects manifested in positional data fitting. Solutions 'a5' (GR) and 'n5' (NG, preferred) are based on data spanning over 1.7 yr in a range of heliocentric distances: 4.93 au – 2.00 au (perihelion) – 3.11 au.
This Oort spike comet suffers tiny planetary perturbations while passing through the planetary system; these perturbations lead to a slightly more tight future orbit, still inside the Oort Cloud (see future barycentric orbits).
| solution description | ||
|---|---|---|
| number of observations | 245 | |
| data interval | 2014 01 04 – 2014 12 30 | |
| data arc selection | data generally limited to pre-perihelion (PRE) | |
| range of heliocentric distances | 4.93 au – 2.13au | |
| detectability of NG effects in the comet's motion | comet with determinable NG~orbit | |
| type of model of motion | GR - gravitational orbit | |
| data weighting | YES | |
| number of residuals | 473 | |
| RMS [arcseconds] | 0.30 | |
| 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] | 26.78 – 28.25 – 29.54 | |
| previous perihelion distance [au] | 213 – 222 – 237 | |
| previous aphelion distance [103 au] | 67.5 – 70.6 – 74.5 | |
| time interval to previous perihelion [Myr] | 6.28 – 6.66 – 7.09 | |
| 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_g 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] | 28.85 – 29.93 – 30.99 | |
| previous perihelion distance [au] | 24 – 29 – 35 | |
| previous aphelion distance [103 au] | 64.5 – 66.8 – 69.3 | |
| time interval to previous perihelion [Myr] | 5.62 – 5.9 – 6.21 | |
| percentage of VCs with qprev > 20 | 100 | |