C/1997 J2 Meunier-Dupouy
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Comet C/1997 J2 was discovered on 7 May 1997 by Michel Meunier (Arbonne la Foret, France) during the observation of comet C/1997 J1 Mueller.Independently, this comet was detected on 8 May by Philippe Dupouy (Observatoire de Dax, France). A day after, Jean Mueller found this comet on the image taken on 5 May (Mount Palomar Observatory)where she discovered C/1997 J1. At the moment of discovery, C/1997 J2 was about 10 months before its perihelion passage and it was last observed in October 1999.
Comet had its closest approach to the Earth on 14 August 1998 (2.492 au), about 5 months after its perihelion passage.
This is a comet with nongravitational effects strongly manifested in positional data fitting.
Solutions given here are based on data spanning over 2.43 yr in a range of heliocentric distances: 4.24 au – 3.05 au (perihelion) – 6.06 au.It is difficult to indicate the preffered non-gravitational orbit and worth noting is also the solution based on g(r)-like formula describing the CO sublimation (solution c1).
This Oort spike comet suffers tiny planetary perturbations during its passage through the planetary system; these perturbations lead to a slightly less tight future orbit.
See also Królikowska 2014 and Królikowska 2020.
Comet had its closest approach to the Earth on 14 August 1998 (2.492 au), about 5 months after its perihelion passage.
This is a comet with nongravitational effects strongly manifested in positional data fitting.
Solutions given here are based on data spanning over 2.43 yr in a range of heliocentric distances: 4.24 au – 3.05 au (perihelion) – 6.06 au.It is difficult to indicate the preffered non-gravitational orbit and worth noting is also the solution based on g(r)-like formula describing the CO sublimation (solution c1).
This Oort spike comet suffers tiny planetary perturbations during its passage through the planetary system; these perturbations lead to a slightly less tight future orbit.
See also Królikowska 2014 and Królikowska 2020.
| solution description | ||
|---|---|---|
| number of observations | 1446 | |
| data interval | 1997 05 05 – 1999 10 09 | |
| data type | perihelion within the observation arc (FULL) | |
| data arc selection | entire data set (STD) | |
| range of heliocentric distances | 4.24 au – 3.05 au (perihelion) – 6.06 au | |
| type of model of motion | NS - non-gravitational orbits for standard g(r) | |
| data weighting | YES | |
| number of residuals | 2863 | |
| RMS [arcseconds] | 0.54 | |
| 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 | 2201 | |
| next reciprocal semi-major axis [10-6 au-1] | -1.55 – 0.22 – 1.97 | |
| next perihelion distance [au] | 86.6 – 88.3 – 89.9 | |
| next aphelion distance [103 au] | 820 – 2000 – 10000 | |
| synchronous stop epoch [Myr] | 2.87 | S |
| percentage of VCs with qnext > 20 | 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 | 0 | |
| no. of escaping VCs in the swarm | 5001 | |
| no. of hyperbolas among escaping VCs in the swarm | 4653 | * |
| next reciprocal semi-major axis [10-6 au-1] | -3.90 – -2.09 – -0.29 | |
| next perihelion distance [au] | 4.18 – 4.23 – 4.28 | |
| next aphelion distance [103 au] | 1300 – 3600 – 19000 | |
| synchronous stop epoch [Myr] | 2.78 | S |
| percentage of VCs with qnext < 10 | 100 | |