Near-parabolic comets split when they were close to perihelion, or objects that have ceased to be observed soon after perihelion passage.
|Comet||qosc||T||Observational arc||No of||Data||Heliocentric||Data||Q*||New||rms [arcsec]||Ref||Data||Preffered||1∕aori||1∕afut|
|name||dates||obs.||span||distance span||type||GR||NG||orbital||/no of||and||selec||solution?||[10−6au−1]|
|C/1999 S4||0.765 a5||20000726||19990927–20000731||1294||0.841||4.33–0.773||pre+||7.5||1a||0.85/2567||new||STD||NO||17.20± 0.86||perished (1)|
Notes. Preferred models are marked in Col.  as “YES”/“’YOS” (orbit based on full data-arc), where preferred NG solution based on g(r)-like function describing CO sublimation is marked as “YOS”, or as “YE1”/“YE2” (for orbit based on pre-perihelion or post perihelion data arc, respectively). An asterisk in Col.  indicates asymmetric NG solution. The last row for each comet presents data used inthe Minor Planet Center and Nakano Notes (if existing) for orbit determination and resulting original and future 1∕a (taken from these websites in March–June 2019). The observational material taken for osculating orbit determination is described in Cols. − and , whereas Cols.  and  give Q* for GR and NG model of motion, respectively, and the resulting orbit quality assessment (orbital class) is given in Col. . The second and third columns show an osculating perihelion distance and perihelion time. The data distribution relative to a perihelion passage is presented in Cols.  and , where “pre” means that all observations were taken before the perihelion passage, “pre+” means that considerably more pre-perihelion measurements were available, and additional “+” means a drastic dominance of data before perihelion. Columns , , and  are explained in Table A.1. (1)See Sekanina (2019). The full table is available at the CDS.
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