C/1996 E1 NEAT
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Comet C/1996 E1 was discovered on 15 March 1996 by Near-Earth-Asteroid Tracking Team (Jet Propulsion Laboratory), that is about 4.5 months before its perihelion passage.This comet was last observed in the mid-October 1996.
Comet had its closest approach to the Earth on 25 September 1996 (1.168 au), about 2 months after its perihelion passage.
This is a comet with nongravitational effects strongly manifested in positional data fitting.
Solutions given here are based on data spanning over 0.578 yr in a range of heliocentric distances: 2.31 au – 1.36 au (perihelion) – 1.76 au.
This Oort spike comet suffers rather moderate planetary perturbations during its passage through the planetary system; these perturbations lead to a more tight future orbit.
See also Królikowska 2014 and Królikowska 2020.
Comet had its closest approach to the Earth on 25 September 1996 (1.168 au), about 2 months after its perihelion passage.
This is a comet with nongravitational effects strongly manifested in positional data fitting.
Solutions given here are based on data spanning over 0.578 yr in a range of heliocentric distances: 2.31 au – 1.36 au (perihelion) – 1.76 au.
This Oort spike comet suffers rather moderate planetary perturbations during its passage through the planetary system; these perturbations lead to a more tight future orbit.
See also Królikowska 2014 and Królikowska 2020.
| solution description | ||
|---|---|---|
| number of observations | 249 | |
| data interval | 1996 03 15 – 1996 10 12 | |
| data type | significantly more measurements before perihelion (PRE+) | |
| data arc selection | entire data set (STD) | |
| range of heliocentric distances | 2.31 au – 1.36 au (perihelion) – 1.76 au | |
| type of model of motion | NS - non-gravitational orbits for standard g(r) | |
| data weighting | YES | |
| number of residuals | 492 | |
| RMS [arcseconds] | 0.60 | |
| orbit quality class | 1b | |
| previous orbit statistics, both Galactic and stellar perturbations were taken into account | ||
|---|---|---|
| no. of returning VCs in the swarm | 4984 | * |
| no. of escaping VCs in the swarm | 17 | |
| no. of hyperbolas among escaping VCs in the swarm | 0 | |
| previous reciprocal semi-major axis [10-6 au-1] | 23.33 – 29.07 – 34.19 | R |
| previous perihelion distance [au] | 1400 – 2100 – 3200 | R |
| previous aphelion distance [103 au] | 57 – 67 – 83 | R |
| time interval to previous perihelion [Myr] | 4.6 – 6 – 8.3 | R |
| 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.
Lower panel (panels): O-C diagram for this(two) solution (solutions) given in this database, where residuals in right ascension are shown using magenta dots and in declination by blue open circles.
Lower panel (panels): O-C diagram for this(two) solution (solutions) given in this database, where residuals in right ascension are shown using magenta dots and in declination by blue open circles.
| previous_g orbit statistics, here only the Galactic tide has been included | ||
|---|---|---|
| no. of returning VCs in the swarm | 4995 | * |
| no. of escaping VCs in the swarm | 6 | |
| no. of hyperbolas among escaping VCs in the swarm | 0 | |
| previous reciprocal semi-major axis [10-6 au-1] | 24.24 – 30.08 – 35.90 | R |
| previous perihelion distance [au] | 3.3 – 11 – 49 | R |
| previous aphelion distance [103 au] | 56 – 66 – 82 | R |
| time interval to previous perihelion [Myr] | 4.6 – 6 – 8.2 | R |
| percentage of VCs with qprev < 10 | 47 | |
| percentage of VCs with 10 < qprev < 20 | 24 | |
| percentage of VCs with qprev > 20 | 29 | |