C/2017 F1 Lemmon
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Comet C/2017 F1 was discovered on 20 March 2017 with Mount Lemmon survey, that is about 8.5 months before its perihelion passage. Later single pre-discovery obsebation was found from 4 February 2017. This comet was rather rarely observed until 18 March 2018.
Comet had its closest approach to the Earth on 24 December 2017 (3.480 au), less than a month after its perihelion passage.
The preferred solution given here is based on data spanning over 1.12 yr in a range of heliocentric distances: 5.10 au – 4.50 au (perihelion) – 4.58 au.
This Oort spike comet suffers moderate planetary perturbations during its passage through the planetary system; these perturbations lead to escape the comet from the planetary zone on a hyperbolic orbit (see future barycentric orbits).
Comet had its closest approach to the Earth on 24 December 2017 (3.480 au), less than a month after its perihelion passage.
The preferred solution given here is based on data spanning over 1.12 yr in a range of heliocentric distances: 5.10 au – 4.50 au (perihelion) – 4.58 au.
This Oort spike comet suffers moderate planetary perturbations during its passage through the planetary system; these perturbations lead to escape the comet from the planetary zone on a hyperbolic orbit (see future barycentric orbits).
solution description | ||
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number of observations | 84 | |
data interval | 2017 03 20 – 2018 02 17 | |
data type | perihelion within the observation arc (FULL) | |
data arc selection | entire data set (STD) | |
range of heliocentric distances | 4.95 au – 4.50 au (perihelion) – 4.54 au | |
detectability of NG effects in the comet's motion | NG effects not determinable | |
type of model of motion | GR - gravitational orbit | |
data weighting | NO | |
number of residuals | 155 | |
RMS [arcseconds] | 0.41 | |
orbit quality class | 1b |
next orbit statistics, both Galactic and stellar perturbations were taken into account | ||
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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] | -277.43 – -270.47 – -263.37 | |
next perihelion distance [au] | 7.984 – 8.063 – 8.141 | |
synchronous stop epoch [Myr] | 1.01 | S |
percentage of VCs with qnext < 10 | 100 |
![](media/img/2017f1/2017f1a1res.png)
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.
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] | -277.30 – -270.34 – -263.25 | |
next perihelion distance [au] | 9.96 – 10.1 – 10.3 | |
synchronous stop epoch [Myr] | 1.02 | S |
percentage of VCs with qnext < 10 | 17 | |
percentage of VCs with 10 < qnext < 20 | 83 |