C/2008 P1 Garradd
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C/2008 P1 was discovered by Gordon J. Garradd on 13 August 2008 on images taken with the 0.5-m Uppsala Schmidt telescope at Siding Spring; its cometary apperance was next confirmed by C. Jacques and E. Pimentel (Belo Horizonte, Minas Gerais, Brazil, 0.30-m reflector) [IAUC 8965, 2008 August 15].
This comet made its closest approach to the Earth on 22 September 2009 (3.028 au), two months after perihelion passage.
Solution given here is based on data spanning over 2.5 yr in a range of heliocentric distances: 4.88 au – 3.896 au (perihelion) – 6.08 au.
This comet suffers small planetary perturbations during its passage through the planetary system that lead to a more tight future orbit (see future barycentric orbit).
See also Królikowska 2014 and Królikowska and Dybczyński 2017.
This comet made its closest approach to the Earth on 22 September 2009 (3.028 au), two months after perihelion passage.
Solution given here is based on data spanning over 2.5 yr in a range of heliocentric distances: 4.88 au – 3.896 au (perihelion) – 6.08 au.
This comet suffers small planetary perturbations during its passage through the planetary system that lead to a more tight future orbit (see future barycentric orbit).
See also Królikowska 2014 and Królikowska and Dybczyński 2017.
| solution description | ||
|---|---|---|
| number of observations | 1373 | |
| data interval | 2008 08 13 – 2011 02 04 | |
| data type | perihelion within the observation arc (FULL) | |
| data arc selection | entire data set (STD) | |
| range of heliocentric distances | 4.88 au – 3.90 au (perihelion) – 6.08 au | |
| detectability of NG effects in the comet's motion | NG effects not determinable | |
| type of model of motion | GR - gravitational orbit | |
| data weighting | YES | |
| number of residuals | 415 | |
| RMS [arcseconds] | 0.61 | |
| orbit quality class | 1a+ | |
| next 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 | |
| next reciprocal semi-major axis [10-6 au-1] | 239.75 – 240.45 – 241.15 | |
| next perihelion distance [au] | 3.90059 – 3.90071 – 3.90083 | |
| next aphelion distance [103 au] | 8.29 – 8.314 – 8.338 | |
| time interval to next perihelion [Myr] | 0.2666 – 0.2677 – 0.2689 | |
| percentage of VCs with qnext < 10 | 100 | |
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.
| next 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 | |
| next reciprocal semi-major axis [10-6 au-1] | 239.77 – 240.47 – 241.17 | |
| next perihelion distance [au] | 3.90469 – 3.90482 – 3.90494 | |
| next aphelion distance [103 au] | 8.289 – 8.313 – 8.337 | |
| time interval to next perihelion [Myr] | 0.2665 – 0.2677 – 0.2689 | |
| percentage of VCs with qnext < 10 | 100 | |