C/2021 C5 PanSTARRS
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Comet C/2021 C5 was discovered on 12 February 2021 with the Pan-STARRS 1 telescope (Haleakala), that is almost two years before its perihelion passage. a few pre-discovery measurements were next found extending the data arc about three weeks back.
Comet had its closest approach to the Earth on 20 June 2023 (2.80 au), more than four months after its perihelion passage.
The preferred NG solution given here ('c5') is based on data span over 3.53 yr in a range of heliocentric distances: 7.43 au – 3.24 au (perihelion) – 5.60 au.
This comet shows visible trends in the O-C distribution for a GR orbit. It is worth noting that, ignoring the existence of NG effects, the last two observations from early July 2024 (after an 11-month data gap) were rejected as poorly fitting the rest of the measurements. The problem disappears for the NG orbit, and these measurements already lie well in the orbit. However, some [O-C] trends are still visible before perihelion in the case of NG solution (first opposition).
This Oort spike comet suffers moderate planetary perturbations during its passage through the planetary system that lead to a more tight future orbit (semimajor axis of about 1,800-1,900 au).
Comet had its closest approach to the Earth on 20 June 2023 (2.80 au), more than four months after its perihelion passage.
The preferred NG solution given here ('c5') is based on data span over 3.53 yr in a range of heliocentric distances: 7.43 au – 3.24 au (perihelion) – 5.60 au.
This comet shows visible trends in the O-C distribution for a GR orbit. It is worth noting that, ignoring the existence of NG effects, the last two observations from early July 2024 (after an 11-month data gap) were rejected as poorly fitting the rest of the measurements. The problem disappears for the NG orbit, and these measurements already lie well in the orbit. However, some [O-C] trends are still visible before perihelion in the case of NG solution (first opposition).
This Oort spike comet suffers moderate planetary perturbations during its passage through the planetary system that lead to a more tight future orbit (semimajor axis of about 1,800-1,900 au).
| solution description | ||
|---|---|---|
| number of observations | 456 | |
| data interval | 2020 12 22 – 2024 07 03 | |
| data type | perihelion within the observation arc (FULL) | |
| data arc selection | entire data set (STD) | |
| range of heliocentric distances | 7.43 au – 3.24 au (perihelion) – 5.6 au | |
| type of model of motion | NC - non-gravitational orbits for symmetric CO-g(r)-like function | |
| data weighting | YES | |
| number of residuals | 895 | |
| 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] | 22.54 – 24.32 – 26.04 | |
| previous perihelion distance [au] | 807.9 – 836 – 843.3 | |
| previous aphelion distance [103 au] | 76 – 81.4 – 87.9 | |
| time interval to previous perihelion [Myr] | 7.2 – 8.1 – 9.1 | |
| percentage of VCs with qprev > 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.
| 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] | 23.11 – 24.99 – 26.88 | |
| previous perihelion distance [au] | 6.1 – 8.9 – 14 | |
| previous aphelion distance [103 au] | 74.4 – 80 – 86.5 | |
| time interval to previous perihelion [Myr] | 7.1 – 7.9 – 8.9 | |
| percentage of VCs with qprev < 10 | 64 | |
| percentage of VCs with 10 < qprev < 20 | 35 | |
| percentage of VCs with qprev > 20 | 1 | |