C/2015 O1 PANSTARRS
more info
Comet C/2015 O1 was discovered on 19 July 2015 with Pan-STARRS 1 telescope (Haleakala), that is about months after its perihelion passage.
Some prediscovery images of this comet were found: taken on 15 and 17 of June 2015 by Space Surveillance Telescope (Atom Site).
Solutions given here are based on data spanning over 4.76 yr in a range of heliocentric distances: 8.65 au – 3.730 au (perihelion) – 7.28 au.
NG orbits using full data-arc as well as independently using pre-perihelion and post-perihelion data are determinable.
See also Królikowska and Dones 2023.
| solution description | ||
|---|---|---|
| number of observations | 2239 | |
| data interval | 2018 02 21 – 2020 03 20 | |
| data arc selection | data generally limited to post-perihelion (POS) | |
| range of heliocentric distances | 3.73 au – 7.28au | |
| type of model of motion | NC - non-gravitational orbits for symmetric CO-g(r)-like function | |
| data weighting | YES | |
| number of residuals | 4459 | |
| RMS [arcseconds] | 0.53 | |
| 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] | 111.83 – 114.85 – 117.78 | |
| next perihelion distance [au] | 3.584 – 3.597 – 3.609 | |
| next aphelion distance [103 au] | 17 – 17.4 – 17.9 | |
| time interval to next perihelion [Myr] | 0.781 – 0.811 – 0.844 | |
| 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 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] | 111.85 – 114.86 – 117.79 | |
| next perihelion distance [au] | 3.569 – 3.583 – 3.595 | |
| next aphelion distance [103 au] | 17 – 17.4 – 17.9 | |
| time interval to next perihelion [Myr] | 0.781 – 0.811 – 0.844 | |
| percentage of VCs with qnext < 10 | 100 | |