C/2014 UN271 Bernardinelli-Bernstein
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The discovery of C/2014 UN271 was announced in June 2021 by Bernardinelli & Bernstein (2021) on the basis of astrometric observations spanning 20 nights from 20 October 2014 to 8 November 2018 (29.0 au–23.7 au from the Sun). A little later, at a heliocentric distance of over 20 au, observers reported the cometary activity of C/2014 UN271.
The comet will pass through perihelion (10.95 au from the Sun) on 22 January 2031; thus solutions given here are currently based on pre-perihelion data taken at large heliocentric distances.
GR solution 'b8' perfectly fits the data; however, GR solution 'd5' based on longer data arc shows that something happened at the end of 2021 because some trend are visible in the period 2010-2020. For example, there may have been some more violent activity associated with the breakaway of a comet fragment as early as late 2021 (heliocentric distance of about 20 au; see [O-C] for the 'ba' solution). These trends in [O-C] indicates that the outburst reported by Kokotanekova et al (2024) was associated with a noticeable action of NG acceleration forces on the comet's motion. This is all the more interesting because it is a very large comet, with a size estimated at 60 km thanks to ALMA and HST observations.
Most probably, this Oort spike comet suffers small planetary perturbations during its passage through the planetary system.
More details about orbital fitting before the year 2022: see Dybczyński and Królikowska (2022)
The comet will pass through perihelion (10.95 au from the Sun) on 22 January 2031; thus solutions given here are currently based on pre-perihelion data taken at large heliocentric distances.
GR solution 'b8' perfectly fits the data; however, GR solution 'd5' based on longer data arc shows that something happened at the end of 2021 because some trend are visible in the period 2010-2020. For example, there may have been some more violent activity associated with the breakaway of a comet fragment as early as late 2021 (heliocentric distance of about 20 au; see [O-C] for the 'ba' solution). These trends in [O-C] indicates that the outburst reported by Kokotanekova et al (2024) was associated with a noticeable action of NG acceleration forces on the comet's motion. This is all the more interesting because it is a very large comet, with a size estimated at 60 km thanks to ALMA and HST observations.
Most probably, this Oort spike comet suffers small planetary perturbations during its passage through the planetary system.
More details about orbital fitting before the year 2022: see Dybczyński and Królikowska (2022)
| solution description | ||
|---|---|---|
| number of observations | 1077 | |
| data interval | 2010 11 15 – 2025 03 11 | |
| data type | observed only before perihelion (PRE) | |
| data arc selection | entire data set (STD) | |
| range of heliocentric distances | 34.07 au – 15.36au | |
| 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 | 2134 | |
| RMS [arcseconds] | 0.30 | |
| orbit quality class | 1a+ | |
| orbital elements (barycentric ecliptic J2000) | ||
|---|---|---|
| Epoch | 2346 08 31 | |
| perihelion date | 2031 01 21.42687248 | ± 0.00365782 |
| perihelion distance [au] | 10.94886019 | ± 0.00002877 |
| eccentricity | 0.99964495 | ± 0.00000402 |
| argument of perihelion [°] | 326.244633 | ± 0.000190 |
| ascending node [°] | 190.008932 | ± 0.000013 |
| inclination [°] | 95.460172 | ± 0.000007 |
| reciprocal semi-major axis [10-6 au-1] | 32.43 | ± 0.37 |
| file containing 5001 VCs swarm |
|---|
| 2014und5.bpl |
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.
Six 2D-projections of the 6D space of future swarm including 5001 VCs. Each density map is given in logarithmic scale presented on the right in the individual panel.