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 |
previous orbit statistics, both Galactic and stellar perturbations were taken into account | ||
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no. of returning VCs in the swarm | 3578 | * |
no. of escaping VCs in the swarm | 1423 | |
no. of hyperbolas among escaping VCs in the swarm | 522 | |
previous reciprocal semi-major axis [10-6 au-1] | -0.39 – 24.39 – 49.46 | |
previous perihelion distance [au] | 35 – 1100 – 3100 | R |
previous aphelion distance [103 au] | 40 – 75 – 270 | |
time interval to previous perihelion [Myr] | 2.6 – 5.3 – 11 | R |
percentage of VCs with qprev < 10 | 9 | |
percentage of VCs with qprev > 20 | 91 |
previous orbit statistics, here only the Galactic tide has been included | ||
---|---|---|
no. of returning VCs in the swarm | 3281 | * |
no. of escaping VCs in the swarm | 1720 | |
no. of hyperbolas among escaping VCs in the swarm | 517 | |
previous reciprocal semi-major axis [10-6 au-1] | -0.31 – 24.42 – 49.46 | |
previous perihelion distance [au] | 1.9 – 9.8 – 250 | R |
previous aphelion distance [103 au] | 40 – 75 – 260 | |
time interval to previous perihelion [Myr] | 2.5 – 5.2 – 11 | R |
percentage of VCs with qprev < 10 | 50 | |
percentage of VCs with 10 < qprev < 20 | 10 | |
percentage of VCs with qprev > 20 | 40 |