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 | 757 | |
data interval | 2000 09 05 – 2002 04 05 | |
data arc selection | data generally limited to pre-perihelion (PRE) | |
range of heliocentric distances | 6.26 au – 3.55au | |
type of model of motion | NH - non-gravitational orbits for water sublimation from subsolar point | |
data weighting | YES | |
number of residuals | 1486 | |
RMS [arcseconds] | 0.54 | |
orbit quality class | 1b |
previous orbit statistics, both Galactic and stellar perturbations were taken into account | ||
---|---|---|
no. of returning VCs in the swarm | 5001 | * |
no. of escaping VCs in the swarm | 0 | |
no. of hyperbolas among escaping VCs in the swarm | 0 | |
previous reciprocal semi-major axis [10-6 au-1] | 65.64 – 68.70 – 71.83 | |
previous perihelion distance [au] | 4.37 – 4.56 – 4.79 | |
previous aphelion distance [103 au] | 27.8 – 29.1 – 30.5 | |
time interval to previous perihelion [Myr] | 1.64 – 1.75 – 1.88 | |
percentage of VCs with qprev < 10 | 100 |
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).
previous orbit statistics, here only the Galactic tide has been included | ||
---|---|---|
no. of returning VCs in the swarm | 5001 | * |
no. of escaping VCs in the swarm | 0 | |
no. of hyperbolas among escaping VCs in the swarm | 0 | |
previous reciprocal semi-major axis [10-6 au-1] | 65.62 – 68.68 – 71.80 | |
previous perihelion distance [au] | 4.2 – 4.32 – 4.46 | |
previous aphelion distance [103 au] | 27.9 – 29.1 – 30.5 | |
time interval to previous perihelion [Myr] | 1.64 – 1.75 – 1.88 | |
percentage of VCs with qprev < 10 | 100 |