C/2020 S3 (Erasmus)
From Cambridge , C/2020 S3 (Erasmus) is not observable – it will reach its highest point in the sky during daytime and is no higher than 5° above the horizon at dawn.
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Name
C/2020 S3 (Erasmus)
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Object type
Comet
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| Computed for: | 02 May 2024 |
| Right ascension: | 00h44m [1] |
| Declination: | +14°48' [1] |
| Constellation: | Pisces |
| Magnitude: | 26.08 (V) [2] |
| Distance: | 13.07 AU 108.73 lightmin [1] |
| Angular motion (speed): | 1.59 deg/yr[1] |
| Angular motion (pos ang): | 264.5° |
| Semi-major axis: | 145.43 AU |
| Eccentricity: | 0.997282 |
| Inclination: | 20.02° |
| Longitude ascending node: | 222.59° |
| Argument of perihelion: | 350.06° |
| Epoch of elements: | 02 May 2024 |
| Mean Anomaly at epoch: | 0.70° |
| Absolute mag (H): | 9.10 [2] |
| Slope parameter (n): | 4.20 [2] |
| Perihelion: | 0.40 AU |
| Aphelion: | 290.46 AU |
| Orbital period: | 1753.77 years |
The position of this comet was calculated from orbital elements published by the Minor Planet Center (MPC).
We estimate the brightnesses of comets from magnitude parameters published by the BAA Comet Section, where these are available. These are computed from the observations they receive from amateur astronomers.
Comets are intrinsically highly unpredictable objects, since their brightness depends on the scattering of sunlight from dust particles in the comet's coma and tail. This dust is continually streaming away from the comet's nucleus, and its density at any particular time is governed by the rate of sublimation of the ice in the comet's nucleus, as it is heated by the Sun's rays. It also depends on the amount of dust that is mixed in with that ice. This is very difficult to predict in advance, and can be highly variable even between successive apparitions of the same comet.
In consequence, while the future positions of comets are usually known with a high degree of confidence, their future brightnesses are not. For most comets, we do not publish any magnitude estimates at all. For the few comets where we do make estimates, we generally prefer the BAA's magnitude parameters to those published by the Minor Planet Center, since they are typically updated more often.