C/1932 M1 Newman
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Comet C/1932 M1 was discovered on 20 June 1932 by K.A. Newman (Lowell Observatory, Arizona, USA) and he found next the prediscovery images on plates exposed on 1 June at the same Observatory.At the moment of discovery, the comet was about three months before perihelion passage, and was last seen on 20 January 1933 [Kronk, Cometography: Volume 3].
This comet made its closest approach to the Earth on 10 June 1932 (1.214 au), that is ten days before its discovery.
Solution given here is based on data spanning over 0.584 yr in a range of heliocentric distances from 2.06 au through perihelion (1.65 au) to 2.25 au.
This Oort spike comet suffers small planetary perturbations during its passage through the planetary system; however, they led to escape the comet from the planetary zone on a hyperbolic orbit (see future barycentric orbit).
More details in Królikowska et al. 2014.
This comet made its closest approach to the Earth on 10 June 1932 (1.214 au), that is ten days before its discovery.
Solution given here is based on data spanning over 0.584 yr in a range of heliocentric distances from 2.06 au through perihelion (1.65 au) to 2.25 au.
This Oort spike comet suffers small planetary perturbations during its passage through the planetary system; however, they led to escape the comet from the planetary zone on a hyperbolic orbit (see future barycentric orbit).
More details in Królikowska et al. 2014.
| solution description | ||
|---|---|---|
| number of observations | 187 | |
| data interval | 1932 06 21 – 1933 01 20 | |
| data type | perihelion within the observation arc (FULL) | |
| data arc selection | entire data set (STD) | |
| range of heliocentric distances | 2.06 au – 1.65 au (perihelion) – 2.25 au | |
| detectability of NG effects in the comet's motion | NG effects not determinable | |
| type of model of motion | GR - gravitational orbit | |
| data weighting | YES | |
| number of residuals | 325 | |
| RMS [arcseconds] | 2.60 | |
| orbit quality class | 1b | |
| 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] | -269.99 – -245.18 – -220.07 | |
| next perihelion distance [au] | 2.13 – 2.22 – 2.32 | |
| synchronous stop epoch [Myr] | 0.972 | S |
| percentage of VCs with qnext < 10 | 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.
| 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] | -270.04 – -245.23 – -220.12 | |
| next perihelion distance [au] | 2.54 – 2.68 – 2.84 | |
| synchronous stop epoch [Myr] | 1 | S |
| percentage of VCs with qnext < 10 | 100 | |