C/2017 E1 Borisov
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Comet C/2017 E1 was discovered on 1 March 2017 by Gennadii Vladimirovich Borisov (Nauchnij, Crimea), that is 1.3 month before its perihelion passage, and was followed until 25 June 2017. Comet had closest approach to the Earth on 18 March 2017 (1.323 au, about three weeks before the perihelion passage).
Only GR orbit is possible to obtain. GR solution given here is based on data spanning over 0.318 yr in a range of heliocentric distances: 1.15 au – 0.901 au (perihelion) – 1.59 au.
This is comet outside the Oort spike with semimajor axis of about 1090 au. Comet suffers notable planetary perturbations during its passage through the planetary system and these perturbations lead to escape the comet from the planetary zone on a hyperbolic orbit (see future barycentric orbit).
GR assumption gives original hyperbolic orbit; however, NG orbit results in original semimajor axis of about 1900–3300 au (uncertainty of one sigma is used).
Only GR orbit is possible to obtain. GR solution given here is based on data spanning over 0.318 yr in a range of heliocentric distances: 1.15 au – 0.901 au (perihelion) – 1.59 au.
This is comet outside the Oort spike with semimajor axis of about 1090 au. Comet suffers notable planetary perturbations during its passage through the planetary system and these perturbations lead to escape the comet from the planetary zone on a hyperbolic orbit (see future barycentric orbit).
GR assumption gives original hyperbolic orbit; however, NG orbit results in original semimajor axis of about 1900–3300 au (uncertainty of one sigma is used).
| solution description | ||
|---|---|---|
| number of observations | 186 | |
| data interval | 2017 03 01 – 2017 06 25 | |
| data type | perihelion within the observation arc (FULL) | |
| data arc selection | entire data set (STD) | |
| range of heliocentric distances | 1.15 au – 0.90 au (perihelion) – 1.59 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 | 365 | |
| RMS [arcseconds] | 0.48 | |
| orbit quality class | 2a | |
| orbital elements (barycentric ecliptic J2000) | ||
|---|---|---|
| Epoch | 1708 05 27 | |
| perihelion date | 2017 04 11.00946085 | ± 0.00009276 |
| perihelion distance [au] | 0.88086682 | ± 0.00000680 |
| eccentricity | 0.99919069 | ± 0.00001300 |
| argument of perihelion [°] | 151.563365 | ± 0.000281 |
| ascending node [°] | 144.511088 | ± 0.000391 |
| inclination [°] | 15.851985 | ± 0.000116 |
| reciprocal semi-major axis [10-6 au-1] | 918.77 | ± 14.76 |
| file containing 5001 VCs swarm |
|---|
| 2017e1a5.bmi |
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.
Middle panel(s): O-C diagram for a given solution (sometimes in comparison to another solution available in CODE), where residuals in right ascension are shown using magenta dots and in declination by blue open circles.
Lowest panel: Relative weights for a given data set(s).
Middle panel(s): O-C diagram for a given solution (sometimes in comparison to another solution available in CODE), where residuals in right ascension are shown using magenta dots and in declination by blue open circles.
Lowest panel: Relative weights for a given data set(s).
Six 2D-projections of the 6D space of original swarm including 5001 VCs. Each density map is given in logarithmic scale presented on the right in the individual panel.