C/2017 B3 LINEAR
more info
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 | 1587 | |
| data interval | 2016 03 04 – 2022 01 01 | |
| data type | perihelion within the observation arc (FULL) | |
| data arc selection | entire data set (STD) | |
| range of heliocentric distances | 9.16 au – 3.92 au (perihelion) – 9.15 au | |
| type of model of motion | NC - non-gravitational orbits for symmetric CO-g(r)-like function | |
| data weighting | YES | |
| number of residuals | 3107 | |
| RMS [arcseconds] | 0.34 | |
| 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] | 298.91 – 299.76 – 300.62 | |
| previous perihelion distance [au] | 3.93027 – 3.93033 – 3.9304 | |
| previous aphelion distance [103 au] | 6.649 – 6.668 – 6.687 | |
| time interval to previous perihelion [Myr] | 0.1915 – 0.1923 – 0.1931 | |
| 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] | 298.91 – 299.77 – 300.62 | |
| previous perihelion distance [au] | 3.9307 – 3.93076 – 3.93083 | |
| previous aphelion distance [103 au] | 6.649 – 6.668 – 6.687 | |
| time interval to previous perihelion [Myr] | 0.1914 – 0.1922 – 0.1931 | |
| percentage of VCs with qprev < 10 | 100 | |