C/2012 F3 PANSTARRS
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Comet C/2012 F3 was discovered by the Pan-STARRS 1 telescope (Haleakala) on 16 March 2012 at a distance of 9.57 au from the Sun.A few pre-discovery images were obtained on 19 January 2012 (9.93 au from the Sun) and 2 March 2012. The comet reached its perihelion almost three years later (3.46 au from the Sun, 6 April 2015), and was followed to 17 October 2017 (8.36 au from the Sun).
C/2012 F3 had its closest approach to the Earth on 7 May 2014 (3.649 au, one month after perihelion passage).
NG orbit using full data-arc as well as using pre-perihelion data are determinable.
This Oort spike comet suffered quite large planetary perturbations during its passage through the planetary system that led to escape the comet from the planetary zone on a hyperbolic orbit (see future barycentric orbit).
See also Królikowska and Dones 2023 and Wysoczańska et al., 2020.
C/2012 F3 had its closest approach to the Earth on 7 May 2014 (3.649 au, one month after perihelion passage).
NG orbit using full data-arc as well as using pre-perihelion data are determinable.
This Oort spike comet suffered quite large planetary perturbations during its passage through the planetary system that led to escape the comet from the planetary zone on a hyperbolic orbit (see future barycentric orbit).
See also Królikowska and Dones 2023 and Wysoczańska et al., 2020.
| solution description | ||
|---|---|---|
| number of observations | 1752 | |
| data interval | 2012 01 19 – 2017 10 17 | |
| data type | perihelion within the observation arc (FULL) | |
| data arc selection | entire data set (STD) | |
| range of heliocentric distances | 9.93 au – 3.46 au (perihelion) – 8.36 au | |
| detectability of NG effects in the comet's motion | comet with NG effects strongly manifested in positional data fitting | |
| type of model of motion | GR - gravitational orbit | |
| data weighting | YES | |
| number of residuals | 3498 | |
| RMS [arcseconds] | 0.55 | |
| 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] | 35.00 – 35.52 – 36.04 | |
| previous perihelion distance [au] | 859 – 883 – 905 | |
| previous aphelion distance [103 au] | 54.6 – 55.4 – 56.2 | |
| time interval to previous perihelion [Myr] | 4.43 – 4.54 – 4.66 | |
| 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] | 35.48 – 36.09 – 36.72 | |
| previous perihelion distance [au] | 2.24 – 2.28 – 2.32 | |
| previous aphelion distance [103 au] | 54.5 – 55.4 – 56.4 | |
| time interval to previous perihelion [Myr] | 4.51 – 4.63 – 4.75 | |
| percentage of VCs with qprev < 10 | 100 | |