C/1886 T1 Barnard-Hartwig
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C/1886 T1 was discovered on 5 October 1886 by Edward Emerson Barnard (Vanderbilt University Observatory, Nashville, Tennessee, USA). Independently, it was discovered on 6 October byErnst Hartwig (Bamberg Observatory, Germany). At the moment of discovery, the comet was about 2.5 months before its perihelion passage and was last seen on 17 June 1887 [Kronk, Cometography: Volume 2].
This comet made its closest approach to the Earth on 5 December 1886 (0.965 au), that is over 3 weeks after perihelion passage.
Solutions given here are based on data spanning over 0.693 yr in a range of heliocentric distances from 1.50 au through perihelion (0.663 au) to 3.01 au.
This Oort spike comet suffers tiny planetary perturbations during its passage through the planetary system; these perturbations lead to a little bit larger future semimajor axis (see future barycentric orbits).
C/1886 T1 was in the original sample of 19 comets used by Oort for his hypothesis on LPCs; however, according to presented here statistics for previous perihelion passage, dynamical status of this comet is uncertain.
See also Królikowska 2020.
This comet made its closest approach to the Earth on 5 December 1886 (0.965 au), that is over 3 weeks after perihelion passage.
Solutions given here are based on data spanning over 0.693 yr in a range of heliocentric distances from 1.50 au through perihelion (0.663 au) to 3.01 au.
This Oort spike comet suffers tiny planetary perturbations during its passage through the planetary system; these perturbations lead to a little bit larger future semimajor axis (see future barycentric orbits).
C/1886 T1 was in the original sample of 19 comets used by Oort for his hypothesis on LPCs; however, according to presented here statistics for previous perihelion passage, dynamical status of this comet is uncertain.
See also Królikowska 2020.
| solution description | ||
|---|---|---|
| number of observations | 320 | |
| data interval | 1886 10 07 – 1887 06 17 | |
| data type | perihelion within the observation arc (FULL) | |
| data arc selection | entire data set (STD) | |
| range of heliocentric distances | 1.5 au – 0.66 au (perihelion) – 3.01 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 | 546 | |
| RMS [arcseconds] | 3.80 | |
| orbit quality class | 2a | |
| next orbit statistics, both Galactic and stellar perturbations were taken into account | ||
|---|---|---|
| no. of returning VCs in the swarm | 2571 | * |
| no. of escaping VCs in the swarm | 2430 | |
| no. of hyperbolas among escaping VCs in the swarm | 1018 | |
| next reciprocal semi-major axis [10-6 au-1] | -9.17 – 16.84 – 41.21 | |
| next perihelion distance [au] | 3.1 – 22 – 220 | R |
| next aphelion distance [103 au] | 46 – 93 – 400 | |
| time interval to next perihelion [Myr] | 3 – 6.2 – 12 | R |
| percentage of VCs with qnext < 10 | 24 | |
| percentage of VCs with 10 < qnext < 20 | 21 | |
| percentage of VCs with qnext > 20 | 55 | |
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.
| next orbit statistics, here only the Galactic tide has been included | ||
|---|---|---|
| no. of returning VCs in the swarm | 2412 | |
| no. of escaping VCs in the swarm | 2589 | * |
| no. of hyperbolas among escaping VCs in the swarm | 1159 | |
| next reciprocal semi-major axis [10-6 au-1] | -11.20 – 15.41 – 40.60 | |
| next perihelion distance [au] | 1.8 – 20 – 360 | R |
| next aphelion distance [103 au] | 46 – 96 – 430 | |
| time interval to next perihelion [Myr] | 3 – 6.2 – 12 | R |
| percentage of VCs with qnext < 10 | 39 | |
| percentage of VCs with 10 < qnext < 20 | 11 | |
| percentage of VCs with qnext > 20 | 50 | |