C/1993 Q1 Mueller
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Comet C/1993 Q1 was discovered on 16 August 1993 by Jean Mueller (Palomar Sky Survey II). Later, a prediscovery image of this comet taken on 28 September 1992 (Palomar Mountain-DSS) was found. At the moment of discovery, this comet was about 7.5 months before its perihelion passage and it was last observed in the mid-April 1994.
Comet had its closest approach to the Earth on 7 May 1994 (0.899 au), 1.5 month after its perihelion passage.
Preferred solution given here is based on data spanning over 1.55 yr in a range of heliocentric distances: 6.51 au – 0.967 au (perihelion) – 1.04 au.
Sekanina (2019) speculates that this comet may not have survived the perihelion passage.
This Oort spike comet suffers small planetary perturbations during its passage through the planetary system; if C/1993 Q1 survived the perihelion passage these perturbations lead to escape the comet on hyperbolic orbit from the planetary zone.
See also Królikowska 2020. .
Comet had its closest approach to the Earth on 7 May 1994 (0.899 au), 1.5 month after its perihelion passage.
Preferred solution given here is based on data spanning over 1.55 yr in a range of heliocentric distances: 6.51 au – 0.967 au (perihelion) – 1.04 au.
Sekanina (2019) speculates that this comet may not have survived the perihelion passage.
This Oort spike comet suffers small planetary perturbations during its passage through the planetary system; if C/1993 Q1 survived the perihelion passage these perturbations lead to escape the comet on hyperbolic orbit from the planetary zone.
See also Królikowska 2020. .
| solution description | ||
|---|---|---|
| number of observations | 536 | |
| data interval | 1992 09 28 – 1994 04 17 | |
| data type | almost all measurements before perihelion (PRE++) | |
| data arc selection | entire data set (STD) | |
| range of heliocentric distances | 6.51 au – 0.97 au (perihelion) – 1.04 au | |
| type of model of motion | NS - non-gravitational orbits for standard g(r) | |
| data weighting | YES | |
| number of residuals | 1063 | |
| RMS [arcseconds] | 0.93 | |
| orbit quality class | 1b | |
| previous orbit statistics, both Galactic and stellar perturbations were taken into account | ||
|---|---|---|
| no. of returning VCs in the swarm | 648 | |
| no. of escaping VCs in the swarm | 4353 | * |
| no. of hyperbolas among escaping VCs in the swarm | 320 | |
| previous reciprocal semi-major axis [10-6 au-1] | 1.28 – 8.88 – 16.55 | |
| previous perihelion distance [au] | 980 – 1200 – 1400 | |
| previous aphelion distance [103 au] | 120 – 210 – 670 | |
| time interval to previous perihelion [Myr] | 2.8 ± 12 | |
| percentage of VCs with qprev > 20 | 100 | |
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.
| previous orbit statistics, here only the Galactic tide has been included | ||
|---|---|---|
| no. of returning VCs in the swarm | 1355 | |
| no. of escaping VCs in the swarm | 3646 | * |
| no. of hyperbolas among escaping VCs in the swarm | 30 | |
| previous reciprocal semi-major axis [10-6 au-1] | 6.24 – 13.03 – 19.78 | |
| previous perihelion distance [au] | 110 – 420 – 880 | R |
| previous aphelion distance [103 au] | 100 – 150 – 310 | |
| time interval to previous perihelion [Myr] | 8.9 – 12 – 14 | R |
| percentage of VCs with qprev > 20 | 100 | |