C/2016 X1 Lemmon
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Comet C/2016 X1 was discovered on 8 December 2016 with the Mount Lemmon survey, that is about 2.3 yr before its perihelion passage. Some prediscovery images of this comet were found: taken on 26 November 2016 by Pan-STARRS 1 telescope (Haleakala). This comet was observed until 23 March 2020.
Comet had its closest approach to the Earth on 13 January 2019 (6.652 au), about 3.5 months before its perihelion passage.
GR solution given here is based on data spanning over 3.32 yr in a range of heliocentric distances: 9.30 au – 7.56 au (perihelion) – 7.84 au.
This comet suffers small planetary perturbations during its passage through the planetary system; this is a long-period comet with original and future semimajor axes of about 3,300 au and 2,000 au, respectively.
#********************************** update of 'Oort spike' comets 2016 - 2020, comet no 3; long-period comet
Comet had its closest approach to the Earth on 13 January 2019 (6.652 au), about 3.5 months before its perihelion passage.
GR solution given here is based on data spanning over 3.32 yr in a range of heliocentric distances: 9.30 au – 7.56 au (perihelion) – 7.84 au.
This comet suffers small planetary perturbations during its passage through the planetary system; this is a long-period comet with original and future semimajor axes of about 3,300 au and 2,000 au, respectively.
#********************************** update of 'Oort spike' comets 2016 - 2020, comet no 3; long-period comet
| solution description | ||
|---|---|---|
| number of observations | 296 | |
| data interval | 2016 11 26 – 2020 03 23 | |
| data type | perihelion within the observation arc (FULL) | |
| data arc selection | entire data set (STD) | |
| range of heliocentric distances | 9.3 au – 7.56 au (perihelion) – 7.84 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 | 573 | |
| RMS [arcseconds] | 0.42 | |
| 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] | 308.53 – 310.12 – 311.70 | |
| previous perihelion distance [au] | 7.5767 – 7.5768 – 7.5769 | |
| previous aphelion distance [103 au] | 6.409 – 6.442 – 6.475 | |
| time interval to previous perihelion [Myr] | 0.1813 – 0.1827 – 0.1841 | |
| percentage of VCs with qprev < 10 | 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] | 308.53 – 310.12 – 311.70 | |
| previous perihelion distance [au] | 7.57564 – 7.57573 – 7.57583 | |
| previous aphelion distance [103 au] | 6.409 – 6.442 – 6.475 | |
| time interval to previous perihelion [Myr] | 0.1813 – 0.1827 – 0.1841 | |
| percentage of VCs with qprev < 10 | 100 | |