C/2017 B3 LINEAR
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Comet C/2017 B3 was discovered on 26 January 2017 with the LINEAR survey, , that is about two years before its perihelion passage. Some prediscovery images of this comet were found: taken on 1 and 10 of Aprilnbsp;2016 by the Pan-STARRS 1 telescope (Haleakala).
Comet had its closest approach to the Earth on 19nbsp;Augustnbsp;2019 (3.480nbsp;au), about a 6.5nbsp;months after its perihelion passage.
Preferred NGnbsp;solution given here is based on data arc spanning over 5.83nbsp;yr in a range of heliocentric distances: 9.16 au – 3.92 au (perihelion) – 9.15 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 2,100 au, respectively.
Comet had its closest approach to the Earth on 19nbsp;Augustnbsp;2019 (3.480nbsp;au), about a 6.5nbsp;months after its perihelion passage.
Preferred NGnbsp;solution given here is based on data arc spanning over 5.83nbsp;yr in a range of heliocentric distances: 9.16 au – 3.92 au (perihelion) – 9.15 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 2,100 au, respectively.
| solution description | ||
|---|---|---|
| number of observations | 1222 | |
| data interval | 2019 03 27 – 2022 01 01 | |
| data arc selection | data generally limited to post-perihelion (POS) | |
| range of heliocentric distances | 3.95 au – 9.15au | |
| type of model of motion | NC - non-gravitational orbits for symmetric CO-g(r)-like function | |
| data weighting | YES | |
| number of residuals | 2413 | |
| RMS [arcseconds] | 0.36 | |
| 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] | 471.30 – 472.63 – 473.96 | |
| next perihelion distance [au] | 3.91112 – 3.91114 – 3.91115 | |
| next aphelion distance [103 au] | 4.216 – 4.228 – 4.24 | |
| time interval to next perihelion [Myr] | 0.09656 – 0.09696 – 0.09737 | |
| percentage of VCs with qnext < 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).
| next_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 | |
| next reciprocal semi-major axis [10-6 au-1] | 471.30 – 472.63 – 473.95 | |
| next perihelion distance [au] | 3.90702 – 3.90704 – 3.90705 | |
| next aphelion distance [103 au] | 4.216 – 4.228 – 4.24 | |
| time interval to next perihelion [Myr] | 0.09656 – 0.09696 – 0.09737 | |
| percentage of VCs with qnext < 10 | 100 | |