C/2013 V1 Boattini
more info
Comet C/2013 V1 was discovered on 4 November 2013 by Andrea Boattini during Catalina Sky Survey, that is almost half a year before its perihelion passage, and was followed until 19 January 2015. C/2013 V1 had close approaches to the Earth on 23 December 2013 (1.47 au, about 1.5 month after the discovery).
This is a comet with NG effects strongly manifested in positional data fitting. Solutions 'a5' and 'n5' (preferred) are based on data spanning over 1.2 yr in a range of heliocentric distances: 2.70 au – 1.661 au (perihelion) – 3.69 au. GR solution 'ba' differ from 'a5' in the method of data weighting, silimarly the pair of NG solutions 'bn' and 'n5'.
This Oort spike comet suffers moderate planetary perturbations while passing through the planetary system; these perturbations lead to escape the comet from the planetary zone on a hyperbolic orbit (see future barycentric orbits) for all orbits given here.
This is a comet with NG effects strongly manifested in positional data fitting. Solutions 'a5' and 'n5' (preferred) are based on data spanning over 1.2 yr in a range of heliocentric distances: 2.70 au – 1.661 au (perihelion) – 3.69 au. GR solution 'ba' differ from 'a5' in the method of data weighting, silimarly the pair of NG solutions 'bn' and 'n5'.
This Oort spike comet suffers moderate planetary perturbations while passing through the planetary system; these perturbations lead to escape the comet from the planetary zone on a hyperbolic orbit (see future barycentric orbits) for all orbits given here.
| solution description | ||
|---|---|---|
| number of observations | 1806 | |
| data interval | 2013 11 04 – 2014 04 18 | |
| data arc selection | data generally limited to pre-perihelion (PRE) | |
| range of heliocentric distances | 2.7 au – 1.66au | |
| detectability of NG effects in the comet's motion | comet with NG effects strongly manifested in positional data fitting | |
| type of model of motion | GR - gravitational orbit | |
| data weighting | YES | |
| number of residuals | 3582 | |
| RMS [arcseconds] | 0.41 | |
| orbit quality class | 1b | |
| 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] | 42.35 – 43.09 – 43.82 | |
| previous perihelion distance [au] | 500 – 590 – 680 | |
| previous aphelion distance [103 au] | 45.1 – 45.8 – 46.5 | |
| time interval to previous perihelion [Myr] | 3.03 – 3.14 – 3.27 | |
| percentage of VCs with qprev > 20 | 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] | 45.23 – 46.48 – 47.66 | |
| previous perihelion distance [au] | 4.79 – 5.16 – 5.62 | |
| previous aphelion distance [103 au] | 42 – 43 – 44.2 | |
| time interval to previous perihelion [Myr] | 3.03 – 3.15 – 3.28 | |
| percentage of VCs with qprev < 10 | 100 | |