 Image of Comet LINEAR (C/2000 WM1) withESO's UVESslit viewer image. | |
| Discovery[1] | |
|---|---|
| Discovered by | LINEAR |
| Discovery date | 16 December 2000 |
| Orbital characteristics[2] | |
| Epoch | 24 January 2002 (JD 2452298.5) |
| Observation arc | 981 days (2.69 years) |
| Earliestprecovery date | 16 November 2000 |
| Number of observations | 2,130 |
| Perihelion | 0.555 AU |
| Eccentricity | 1.00024 |
| Inclination | 72.55° |
| 239.89° | |
| Argument of periapsis | 276.77° |
| Mean anomaly | 0.000012° |
| Last perihelion | 22 January 2002 |
| EarthMOID | 0.013 AU |
| JupiterMOID | 2.896 AU |
| Physical characteristics[3] | |
| Dimensions | 3.4–4.0 km (2.1–2.5 mi) |
Mean diameter | 3.8 km (2.4 mi) |
| Comet total magnitude (M1) | 11.2 |
| 2.5 (2002 apparition) | |
C/2000 WM1 (LINEAR) is anon-periodic comet discovered byLINEAR on 16 December 2000. The comet brightened to anapparent magnitude of about 2.5.[4]
The comet was discovered on 16 December 2000 by theLINEAR team. It looked like anasteroid with an apparent magnitude of 17.8. It was also found in images obtained by LINEAR on 16 and 18 November 2000, when it had a magnitude of 18.[1]Timothy Bruce Spahr observed the object with the 1.2-mreflector telescope of theSmithsonian Astrophysical Observatory and found it had a coma 10 arcseconds across and a broad, faint tail that was 10-20 arcseconds long.[1] Theephemeris published upon discovery predicted it would a reach a magnitude of around 4 in early January 2000, and thus become visible with the naked eye.[5]
The comet by late August 2001 had brightened to an apparent magnitude of 14 and in late September its magnitude was estimated to be 11.5 based on visual observations.[6] On 14 November the comet was reported to have an apparent magnitude 7.2 and atail 1.1 degrees long was visible with 10×50binoculars. On 3 December the comet had brightened to a magnitude of 5.3 and its coma had an estimated diameter of 21 arcminutes.[7]
The comet approached Earth at a distance of 0.316 AU (47.3 million km; 29.4 million mi) on 2 December 2001, on its way to perihelion.[2] After mid December it became more easily observed from the southern hemisphere.[8] The comet had an estimated magnitude of 6 in early January 2002, but around perihelion it experienced an outburst and on 27 January, five days after perihelion, brightened to a magnitude 4.6.[9] Two days later its apparent magnitude was reported to be 2.8 to 3.[10] Its tail was reported to be several degrees long.[8] The comet then faded following the predicted curve. In late March 2002, when its magnitude was reported to be 9–10, it became visible from the northern hemisphere again.[8]
The comet was last observed on 8 August 2002, when it had an apparent magnitude of 14.[8]
Thespectrum of C/2000 WM1 was obtained innear infrared by the Near Infrared Echelle Spectrograph (NIRSPEC) atKeck-2 Observatory on 23–25 November 2001, as the comet approached the Sun. The comet has been found to be depleted inmethanol andcarbon monoxide relative to water. CO andacetylene were considerably depleted when compared withOort cloud comets, whilehydrogen cyanide,methane andmethanol were moderately depleted.[11] The radio spectrum of the comet also indicated it was depleted in CO andhydrogen sulfide.[12] The cause of this has been suggested to be that the comet formed closer to the Sun than the Oort cloud comets and was later ejected to the Oort cloud.[11]
Other spectrographic studies have founddiatomic carbon (C2),triatomic carbon (C3),cyanide (CN),amino radical (NH2), water cation, and maybe diatomic carbon anion.[13] The spectrum obtained on 1 December 2001 with the Fiber fed Extended Range Optical Spectrograph (FEROS) of ESO also revealed the presence ofmethylidyne radical (CH) neutral molecule and cation, and CO+.[14][15] The CN production rate was estimated to be2.43×1026 molecules per second and C2 production rate was3.1×1026 molecules per second on 2–4 December 2001, indicated that the comet is relatively enriched in diatomic carbon.[16] The ratio ofhydrogen cyanide (HCN) andhydrogen isocyanide (HNC) was HNC/HCN = 0.09–0.19, similar to that of153P/Ikeya-Zhang.[17]
The UVES spectrograph on the 8.2-mVery Large Telescope KUEYEN was used to obtain theultraviolet-visual spectrum of the comet in mid-March 2002, after perihelion. Of particular interest is the unambiguous detection and measurement of thenitrogen-15isotope. The only other comet in which this isotope had been observed until then wasComet Hale-Bopp. The isotopic abundance ratio was the same in both comets, about 1 nitrogen-15 atom for each 140 nitrogen-14 atoms (14 N/15 N =140±30), which is about half of the terrestrial value (272). On the other hand, the 12 C/13 C isotopic ratio was115±20, close to the "standard" solar system value of 89.[18]
The dust coma was symmetrical before perihelion along the Sun-comet axis, with a tail and a sunward structure with projected length of about 20,000 kilometers, but when imaging CN, a faint and double-jet structure with projected length of 11,500 km (7,100 mi).[16] On 13 December 2001 the water production was estimated to be5.2×1028 molecules per second, indicating an active sublimation area of 10 km2 and thus a nucleus with a diameter of at least 1.8 km (1.1 mi).[19]
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