C/2013 V5 Qukaimeden
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Comet C/2013 V5 was discovered on 12 November 2013 by Michel Ory, Qukaimeden Observatory Marrakech, that is about 10.5 months before its perihelion passage, and was followed until 19 April 2015. C/2013 V5 had close approach to the Earth on 16 September 2014 (0.481 au, about 12 days before the perihelion passage).
This is comet with NG effects strongly manifested in positional data fitting, especially since a few weeks before perihelion passage on September 28 (2014). This is tightly 'correlated with the observations from FRAM telescope : on September 12 the telescope recorded a small outburst after what the scientists observed a dramatic decline in comet magnitude and its dust production, which dropped by factor 5 from outburst level and 2.5 from pre-outburst activity. During orbit modeling, several characteristic behaviors are also observed, which can be traced using [O-C] associated with the descriptions of GR (a5) and NG (n5) solutions.It is worth emphasizing here that positional observations after October 20 (more than a month after the perihelion passage) are automatically rejected when determining the NG orbit (with constant NG parameters). Such behaviors confirm the high probability of at least partial depletion of the mass of the comet nucleus.
Solution 'n5' (preferred) is based on data spanning over 0.94 yr in a range of heliocentric distances: 4.60 au – 0.625 au (perihelion) – 0.79 au. We also give solutions based on the entire post-perihelion leg of orbits for comparison with pre-perihelion orbit, especially to show that NG parameters increased tremendously compared with those obtained for pre-perihelion NG orbit. This is most likely due to the large loss of nucleus mass after perihelion.
This Oort spike comet suffers large planetary perturbations while passing through the planetary system. Assuming that the comet survived the perihelion passage these perturbations can lead to significantly more tight orbit with a semimajor axis of about 330 au (see future barycentric orbit for solution 'r1' or 'rn', that is based on postperihelion data arc).
This is comet with NG effects strongly manifested in positional data fitting, especially since a few weeks before perihelion passage on September 28 (2014). This is tightly 'correlated with the observations from FRAM telescope : on September 12 the telescope recorded a small outburst after what the scientists observed a dramatic decline in comet magnitude and its dust production, which dropped by factor 5 from outburst level and 2.5 from pre-outburst activity. During orbit modeling, several characteristic behaviors are also observed, which can be traced using [O-C] associated with the descriptions of GR (a5) and NG (n5) solutions.It is worth emphasizing here that positional observations after October 20 (more than a month after the perihelion passage) are automatically rejected when determining the NG orbit (with constant NG parameters). Such behaviors confirm the high probability of at least partial depletion of the mass of the comet nucleus.
Solution 'n5' (preferred) is based on data spanning over 0.94 yr in a range of heliocentric distances: 4.60 au – 0.625 au (perihelion) – 0.79 au. We also give solutions based on the entire post-perihelion leg of orbits for comparison with pre-perihelion orbit, especially to show that NG parameters increased tremendously compared with those obtained for pre-perihelion NG orbit. This is most likely due to the large loss of nucleus mass after perihelion.
This Oort spike comet suffers large planetary perturbations while passing through the planetary system. Assuming that the comet survived the perihelion passage these perturbations can lead to significantly more tight orbit with a semimajor axis of about 330 au (see future barycentric orbit for solution 'r1' or 'rn', that is based on postperihelion data arc).
| solution description | ||
|---|---|---|
| number of observations | 1486 | |
| data interval | 2013 11 12 – 2014 10 20 | |
| data type | perihelion within the observation arc (FULL) | |
| data arc selection | entire data set (STD) | |
| range of heliocentric distances | 4.6 au – 0.62 au (perihelion) – 0.79 au | |
| type of model of motion | NS - non-gravitational orbits for standard g(r) | |
| data weighting | YES | |
| number of residuals | 2942 | |
| RMS [arcseconds] | 0.35 | |
| orbit quality class | 1b | |
| orbital elements (heliocentric ecliptic J2000) | ||
|---|---|---|
| Epoch | 2014 12 09 | |
| perihelion date | 2014 09 28.22267149 | ± 0.00002728 |
| perihelion distance [au] | 0.62545118 | ± 0.00000137 |
| eccentricity | 0.99852694 | ± 0.00000684 |
| argument of perihelion [°] | 314.570188 | ± 0.000164 |
| ascending node [°] | 278.616914 | ± 0.000064 |
| inclination [°] | 154.88421 | ± 0.000025 |
| reciprocal semi-major axis [10-6 au-1] | 2,355.19 | ± 10.93 |
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).
| non-gravitational parameters | ||
|---|---|---|
| A1 [10-8au/day2] | 1.4375 | ± 0.051 |
| A2 [10-8au/day2] | -0.71707 | ± 0.03499 |
| A3 [10-8au/day2] | -0.26044 | ± 0.01467 |
| m | -2.15 | |
| n | 5.093 | |
| k | -4.6142 | |
| r0 [au] | 2.808 | |
| α | 0.1113 | |