C/2019 Q1 Lemmon
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Comet C/2019 Q1 was discovered on 28 August 2019, almost one year before its perihelion passage. Later two series of pre-discovery observations were found from 2 January 2019 and 10 November 2018. This comet was observed until 4 June 2021.
Comet had its closest approach to the Earth on 3 September 2020 (4.09 au); 1.5 month after its perihelion passage.
Solutions (GR and NG) given here are based on data span over 2.56 yr in a range of heliocentric distances: 6.80 au – 5.00 au (perihelion) – 5.56 au. Orbits based on pre-perihelion and post-perihelion data independently were also obtained.
This Oort spike comet suffers small planetary perturbations during its passage through the planetary system; however, they lead to escape this comet from the solar system on hyperbolic orbit (see future barycentric orbits).
Comet had its closest approach to the Earth on 3 September 2020 (4.09 au); 1.5 month after its perihelion passage.
Solutions (GR and NG) given here are based on data span over 2.56 yr in a range of heliocentric distances: 6.80 au – 5.00 au (perihelion) – 5.56 au. Orbits based on pre-perihelion and post-perihelion data independently were also obtained.
This Oort spike comet suffers small planetary perturbations during its passage through the planetary system; however, they lead to escape this comet from the solar system on hyperbolic orbit (see future barycentric orbits).
| solution description | ||
|---|---|---|
| number of observations | 249 | |
| data interval | 2018 11 10 – 2021 06 04 | |
| data type | perihelion within the observation arc (FULL) | |
| data arc selection | entire data set (STD) | |
| range of heliocentric distances | 6.8 au – 5.00 au (perihelion) – 5.56 au | |
| 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 | 487 | |
| RMS [arcseconds] | 0.35 | |
| 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] | 31.85 – 33.09 – 34.35 | |
| previous perihelion distance [au] | 800 – 830 – 856 | |
| previous aphelion distance [103 au] | 57.4 – 59.6 – 61.9 | |
| time interval to previous perihelion [Myr] | 5.02 – 5.29 – 5.57 | |
| 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] | 32.68 – 33.77 – 34.87 | |
| previous perihelion distance [au] | 5.6 – 6.6 – 8 | |
| previous aphelion distance [103 au] | 57.4 – 59.2 – 61.2 | |
| time interval to previous perihelion [Myr] | 4.79 – 5.02 – 5.26 | |
| percentage of VCs with qprev < 10 | 99 | |
| percentage of VCs with 10 < qprev < 20 | 1 | |