C/2014 B1 Schwartz
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Comet C/2014 B1 was discovered on 28 January 2014 with Tenagra Observatory near Nogales (U.S.A.), that is about 3.8 yr before its perihelion passage. This comet was observed until the end of 2019, and is still observable.
Comet had its closest approach to the Earth on 23 February 2018 (8.613 au), about 5.5 months after its perihelion passage. Similar close approach to the Earth was at the previous opposition on 11 February 2017 (8.664 au).
Solution given here is based on data spanning over 4.07 yr in a range of heliocentric distances: 11.97 au – 9.557 au (perihelion) – 9.60 au (23 February 2018).
This Oort spike comet suffers extremely slight planetary perturbations during its passage through the planetary system and its semimajor axis will be almost unchanged after leaving the planetary zone (see future barycentric orbits).
Comet had its closest approach to the Earth on 23 February 2018 (8.613 au), about 5.5 months after its perihelion passage. Similar close approach to the Earth was at the previous opposition on 11 February 2017 (8.664 au).
Solution given here is based on data spanning over 4.07 yr in a range of heliocentric distances: 11.97 au – 9.557 au (perihelion) – 9.60 au (23 February 2018).
This Oort spike comet suffers extremely slight planetary perturbations during its passage through the planetary system and its semimajor axis will be almost unchanged after leaving the planetary zone (see future barycentric orbits).
| solution description | ||
|---|---|---|
| number of observations | 689 | |
| data interval | 2014 01 28 – 2018 02 23 | |
| data type | perihelion within the observation arc (FULL) | |
| data arc selection | entire data set (STD) | |
| range of heliocentric distances | 11.97 au – 9.56 au (perihelion) – 9.6 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 | 1339 | |
| RMS [arcseconds] | 0.29 | |
| 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] | 60.41 – 61.07 – 61.71 | |
| previous perihelion distance [au] | 12.91 – 13.02 – 13.14 | |
| previous aphelion distance [103 au] | 32.4 – 32.7 – 33.1 | |
| time interval to previous perihelion [Myr] | 2.05 – 2.09 – 2.12 | |
| percentage of VCs with 10 < qprev < 20 | 100 | |
| previous 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] | 60.40 – 61.07 – 61.71 | |
| previous perihelion distance [au] | 12.43 – 12.54 – 12.67 | |
| previous aphelion distance [103 au] | 32.4 – 32.7 – 33.1 | |
| time interval to previous perihelion [Myr] | 2.06 – 2.09 – 2.12 | |
| percentage of VCs with 10 < qprev < 20 | 100 | |