C/2015 R3 PANSTARRS
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Comet C/2015 R3 was discovered on 12 September 2015 with Pan-STARRS 1 telescope (Haleakala), that is about 1.6 yr after its perihelion passage. After some time pre-discovery data were found going back to 5 March 2013. This comet was rarely observed until 28 September 2016.
Comet had its closest approach to the Earth on 8 May 2015 (4.939 au), a week after its perihelion passage.
We recommended GR solution spanning over 3.57 yr in a range of heliocentric distances from 5.57 au – 4.90 au (perihelion) – 8.54 au as the preferred orbit( solution 'b1'), because radial component of NG~acceleration is negative in solution 'bc'.
This Oort spike comet suffers small planetary perturbations during its passage through the planetary system that lead to a more tight future orbit with a semimajor axis larger than 10000 au (see future barycentric orbits).
Comet had its closest approach to the Earth on 8 May 2015 (4.939 au), a week after its perihelion passage.
We recommended GR solution spanning over 3.57 yr in a range of heliocentric distances from 5.57 au – 4.90 au (perihelion) – 8.54 au as the preferred orbit( solution 'b1'), because radial component of NG~acceleration is negative in solution 'bc'.
This Oort spike comet suffers small planetary perturbations during its passage through the planetary system that lead to a more tight future orbit with a semimajor axis larger than 10000 au (see future barycentric orbits).
| solution description | ||
|---|---|---|
| number of observations | 44 | |
| data interval | 2013 03 05 – 2016 09 28 | |
| data type | perihelion within the observation arc (FULL) | |
| data arc selection | entire data set (STD) | |
| range of heliocentric distances | 5.57 au – 4.90 au (perihelion) – 8.54 au | |
| type of model of motion | NC - non-gravitational orbits for symmetric CO-g(r)-like function | |
| data weighting | YES | |
| number of residuals | 83 | |
| RMS [arcseconds] | 0.52 | |
| orbit quality class | 1a | |
| previous orbit statistics, both Galactic and stellar perturbations were taken into account | ||
|---|---|---|
| no. of returning VCs in the swarm | 578 | |
| no. of escaping VCs in the swarm | 4423 | |
| no. of hyperbolas among escaping VCs in the swarm | 3583 | * |
| previous reciprocal semi-major axis [10-6 au-1] | -57.50 – -17.66 – 21.24 | |
| previous perihelion distance [au] | 8.6 – 11 – 14 | |
| previous aphelion distance [103 au] | 50 – 130 – 720 | |
| time interval to previous perihelion [Myr] | 1.43 ± 3.2 | |
| percentage of VCs with qprev < 10 | 30 | |
| percentage of VCs with 10 < qprev < 20 | 70 | |
| previous orbit statistics, here only the Galactic tide has been included | ||
|---|---|---|
| no. of returning VCs in the swarm | 667 | |
| no. of escaping VCs in the swarm | 4334 | |
| no. of hyperbolas among escaping VCs in the swarm | 3583 | * |
| previous reciprocal semi-major axis [10-6 au-1] | -57.44 – -17.61 – 21.27 | |
| previous perihelion distance [au] | 7.9 – 10 – 13 | |
| previous aphelion distance [103 au] | 50 – 130 – 720 | |
| time interval to previous perihelion [Myr] | 1.46 ± 3.2 | |
| percentage of VCs with qprev < 10 | 48 | |
| percentage of VCs with 10 < qprev < 20 | 52 | |