C/2015 VL62 Lemmon-Yeung-PanSTARRS
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The discovery of comet C/2015 VL62 was officially attributed to three groups: Mt Lemmon Survey (R. G. Matheny and E. J. Christensen), W. K. Y. Yeung (near Mayhill, NM, USA), and Pan-STARRS 1 telescope (Haleakala). Comet was observed around four oppositions until 16 July 2018. C/2015 VL62 had closest approach to the Earth on 21 August 2017 (1.74 au, about a week before the perihelion passage).
This is a comet with NG effects determinable using positional data fitting. Solutions 'a5' and 'n5' (preferred) are based on data spanning over 2.70 yr in a range of heliocentric distances: 6.72 au – 2.720 au (perihelion) – 4.21 au. GR solution 'ba' differ from 'a5' in the method of data weighting, silimarly the pair of NG solutions 'bn' and 'n5', and 'pn' and 'pe' ((the last pair of NG solutions is based on pre-perihelion data arc). NG parameters are better determined for solutions 'bn' than the 'n5'. However, in both solutions are still visible tiny trends in [O-C]. In our opinion, the better is [O-C] for the solution 'n5', especially in the first and last opposition. Thus, we suggest this solution be treated as preferred. Alternatively, the solution 'pe' (based on the pre-perihelion orbital leg) can also be taken for the study of the origin of this comet.
This Oort Cloud comet suffers moderate planetary perturbations while passing through the planetary system; these perturbations lead to escape the comet from the planetary zone on a hyperbolic orbit (see future barycentric orbits for all orbits given here).
This is a comet with NG effects determinable using positional data fitting. Solutions 'a5' and 'n5' (preferred) are based on data spanning over 2.70 yr in a range of heliocentric distances: 6.72 au – 2.720 au (perihelion) – 4.21 au. GR solution 'ba' differ from 'a5' in the method of data weighting, silimarly the pair of NG solutions 'bn' and 'n5', and 'pn' and 'pe' ((the last pair of NG solutions is based on pre-perihelion data arc). NG parameters are better determined for solutions 'bn' than the 'n5'. However, in both solutions are still visible tiny trends in [O-C]. In our opinion, the better is [O-C] for the solution 'n5', especially in the first and last opposition. Thus, we suggest this solution be treated as preferred. Alternatively, the solution 'pe' (based on the pre-perihelion orbital leg) can also be taken for the study of the origin of this comet.
This Oort Cloud comet suffers moderate planetary perturbations while passing through the planetary system; these perturbations lead to escape the comet from the planetary zone on a hyperbolic orbit (see future barycentric orbits for all orbits given here).
| solution description | ||
|---|---|---|
| number of observations | 304 | |
| data interval | 2017 08 28 – 2018 07 16 | |
| data arc selection | data generally limited to pre-perihelion (PRE) | |
| range of heliocentric distances | 2.72 au – 2.72 au (perihelion) – 4.21 au | |
| detectability of NG effects in the comet's motion | comet with determinable NG~orbit | |
| type of model of motion | GR - gravitational orbit | |
| data weighting | YES | |
| number of residuals | 595 | |
| RMS [arcseconds] | 0.42 | |
| orbit quality class | 1b | |
| orbital elements (barycentric ecliptic J2000) | ||
|---|---|---|
| Epoch | 2312 12 07 | |
| perihelion date | 2017 08 29.14450236 | ± 0.00020768 |
| perihelion distance [au] | 2.70552538 | ± 0.00000211 |
| eccentricity | 1.00145442 | ± 0.00000282 |
| argument of perihelion [°] | 128.764242 | ± 0.000080 |
| ascending node [°] | 95.184143 | ± 0.000037 |
| inclination [°] | 165.831131 | ± 0.000012 |
| reciprocal semi-major axis [10-6 au-1] | -537.57 | ± 1.04 |
| file containing 5001 VCs swarm |
|---|
| 2015vlra.bpl |
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 future swarm including 5001 VCs. Each density map is given in logarithmic scale presented on the right in the individual panel.