C/1999 H3 LINEAR
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C/1999 H3 was discovered as an apparently asteroidal object by LINEAR on 22 April 1999 (about four months before perihelion passage). Next day was reported as cometary object by observers from Klet and Ondrejov [IAUC 7151, 1999 April 23].
This comet made its closest approach to Earth on 6 March 2000 (3.185 au), about 7.5 months after perihelion.
Solution given here is based on data span over 2.9 yr in a range of heliocentric distances: 3.66 au – 3.501 au (perihelion) – 8.48 au.
NG orbits using full data-arc as well as using post-perihelion data are determinable.
See also Królikowska and Dones 2023, Królikowska and Dybczyński 2017,and Królikowska 2014.
This comet made its closest approach to Earth on 6 March 2000 (3.185 au), about 7.5 months after perihelion.
Solution given here is based on data span over 2.9 yr in a range of heliocentric distances: 3.66 au – 3.501 au (perihelion) – 8.48 au.
NG orbits using full data-arc as well as using post-perihelion data are determinable.
See also Królikowska and Dones 2023, Królikowska and Dybczyński 2017,and Królikowska 2014.
| solution description | ||
|---|---|---|
| number of observations | 877 | |
| data interval | 1999 04 22 – 2002 03 20 | |
| data type | significantly more measurements after perihelion (POST+) | |
| data arc selection | entire data set (STD) | |
| range of heliocentric distances | 3.66 au – 3.50 au (perihelion) – 8.48 au | |
| type of model of motion | NS - non-gravitational orbits for standard g(r) | |
| data weighting | YES | |
| number of residuals | 1722 | |
| RMS [arcseconds] | 0.51 | |
| orbit quality class | 1a | |
| next orbit statistics, both Galactic and stellar perturbations were taken into account | ||
|---|---|---|
| no. of returning VCs in the swarm | 0 | |
| no. of escaping VCs in the swarm | 5001 | |
| no. of hyperbolas among escaping VCs in the swarm | 5001 | * |
| next reciprocal semi-major axis [10-6 au-1] | -9.85 – -8.53 – -7.20 | |
| next perihelion distance [au] | 108.9 – 110 – 111.1 | |
| synchronous stop epoch [Myr] | 2.6 | S |
| percentage of VCs with qnext > 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).
| next orbit statistics, here only the Galactic tide has been included | ||
|---|---|---|
| no. of returning VCs in the swarm | 0 | |
| no. of escaping VCs in the swarm | 5001 | |
| no. of hyperbolas among escaping VCs in the swarm | 5001 | * |
| next reciprocal semi-major axis [10-6 au-1] | -10.09 – -8.77 – -7.44 | |
| next perihelion distance [au] | 5.4 – 5.8 – 6.21 | |
| synchronous stop epoch [Myr] | 2.63 | S |
| percentage of VCs with qnext < 10 | 100 | |