C/2000 SV74 LINEAR
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Comet C/2000 SV74 was discovered on 24 September 2009 by LINEAR as an apparently asteroidal object; CCD images taken by Milos Tichy (Klet Observatory) on 19 October 2000 revealed a cometary appearance [[IAUC 7510, 2000 October 19]. Later, five images of this object were found on LINEAR exposures taken on 5 September 2000. Comet passed perihelion at the end of April 2002.
C/2000 SV74 was observed 4.7 yr in a range of heliocentric distances: 6.26 au – 3.542 au (perihelion) – 9.51 au.
Comet had its closest approach to Earth on 3 November 2001 (3.195 au, six months before perihelion).
Nongravitational solution bbased on entire data arc still reveals some trends in (O-C) where most evident are in the last opposition; NG orbits independently using pre-perihelion and post-perihelion data are also determinable.
Nakano non-gravitational solution [ Nakano Notes 1258] also shows trends in (O-C) in the last opposition. This solution, derived by T. Kobayashi, is based on 2116 observations (arc: 2000 September 5 to 2005 April 15; rms = 0.60 arcsec) and the NG-effects of sublimating CO-molecule (or N2) using Yabushita's theory (MNRAS 283, 347), and gives 1/aorigin = +0.000074, 1/afuture = -0.000073).
See also Królikowska and Dones 2023 and Królikowska and Dybczyński 2017.
C/2000 SV74 was observed 4.7 yr in a range of heliocentric distances: 6.26 au – 3.542 au (perihelion) – 9.51 au.
Comet had its closest approach to Earth on 3 November 2001 (3.195 au, six months before perihelion).
Nongravitational solution bbased on entire data arc still reveals some trends in (O-C) where most evident are in the last opposition; NG orbits independently using pre-perihelion and post-perihelion data are also determinable.
Nakano non-gravitational solution [ Nakano Notes 1258] also shows trends in (O-C) in the last opposition. This solution, derived by T. Kobayashi, is based on 2116 observations (arc: 2000 September 5 to 2005 April 15; rms = 0.60 arcsec) and the NG-effects of sublimating CO-molecule (or N2) using Yabushita's theory (MNRAS 283, 347), and gives 1/aorigin = +0.000074, 1/afuture = -0.000073).
See also Królikowska and Dones 2023 and Królikowska and Dybczyński 2017.
| solution description | ||
|---|---|---|
| number of observations | 1450 | |
| data interval | 2002 05 02 – 2005 05 12 | |
| data arc selection | data generally limited to post-perihelion (POS) | |
| range of heliocentric distances | 3.54 au – 9.51au | |
| detectability of NG effects in the comet's motion | comet with NG effects strongly manifested in positional data fitting | |
| type of model of motion | GR - gravitational orbit | |
| data weighting | YES | |
| number of residuals | 2879 | |
| RMS [arcseconds] | 0.70 | |
| orbit quality class | 1a+ | |
| orbital elements (heliocentric ecliptic J2000) | ||
|---|---|---|
| Epoch | 2002 05 06 | |
| perihelion date | 2002 04 30.45713736 | ± 0.00030433 |
| perihelion distance [au] | 3.54157522 | ± 0.00000264 |
| eccentricity | 1.00484841 | ± 0.00000208 |
| argument of perihelion [°] | 76.222572 | ± 0.000069 |
| ascending node [°] | 24.185147 | ± 0.000013 |
| inclination [°] | 75.237036 | ± 0.000012 |
| reciprocal semi-major axis [10-6 au-1] | -1,369.00 | ± 0.59 |
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).