 Comet McNaught as seen from Swift's Creek,Victoria on 23 January 2007 | |
| Discovery | |
|---|---|
| Discovered by | Robert H. McNaught |
| Discovery site | Siding Spring Observatory (Uppsala Southern Schmidt Telescope) |
| Discovery date | 7 August 2006 |
| Orbital characteristics[2][3][4] | |
| Epoch | 26 November 2006 (JD 2454065.5) |
| Observation arc | 338 days |
| Number of observations | 331 |
| Orbit type | Oort cloud |
| Aphelion | ~67,000 AU (inbound) ~4,100 AU (outbound) |
| Perihelion | 0.171 AU |
| Semi-major axis | ~33,000 AU (inbound) ~2,000 AU (outbound) |
| Eccentricity | 1.000019 (inbound) 0.99917 (outbound) |
| Orbital period | ~6 million years (inbound) ~92,600 years (outbound) |
| Max.orbital speed | 101.9 km/s (63.3 mi/s)[1] |
| Inclination | 77.837° |
| 267.41° | |
| Argument of periapsis | 155.97° |
| Last perihelion | 12 January 2007 |
| EarthMOID | 0.409 AU |
| JupiterMOID | 0.316 AU |
| Physical characteristics[5][7] | |
Mean radius | 1.58 km (0.98 mi)[a] |
| 21 hours | |
| Comet total magnitude (M1) | 5.4 |
| Comet nuclear magnitude (M2) | 12.9 |
| –5.5 (2007 apparition)[6] | |
Comet McNaught, also known as theGreat Comet of 2007 andgiven the designationC/2006 P1, is anon-periodic comet discovered on 7 August 2006 by British-Australian astronomerRobert H. McNaught using theUppsala Southern Schmidt Telescope.[8] It was the brightest comet in over 40 years, and was easily visible to thenaked eye for observers in theSouthern Hemisphere in January and February 2007.
With an estimated peakmagnitude of −5.5, the comet was the second-brightest since 1935.[6] Aroundperihelion on 12 January, it was visible worldwide in broad daylight. Its tail measured an estimated at 74.935 million km (0.501 AU) in length and stretched 35 degrees across the sky at its peak.[9]
The brightness of C/2006 P1 near perihelion was enhanced byforward scattering.[10]
McNaught discovered the comet in aCCD image on 7 August 2006 during the course of routine observations for theSiding Spring Survey, which searched for Near-Earth Objects that might represent a collision threat to Earth. The comet was discovered inOphiuchus, shining very dimly at a magnitude of about +17. From August through November 2006, the comet was imaged and tracked as it moved through Ophiuchus andScorpius, brightening as high asmagnitude +9, still too dim to be seen with the unaided eye.[9] Then, for most of December, the comet was lost in the glare of theSun.[citation needed]
Upon recovery, it became apparent that the comet was brightening very fast, reaching naked-eye visibility in early January 2007. It was visible to northern hemisphere observers, inSagittarius and surrounding constellations, until about 13 January. Perihelion was 12 January at a distance of 0.17 AU (25 million km). This was close enough to the Sun to be observed by the space-basedSolar and Heliospheric Observatory (SOHO).[11] The comet entered SOHO'sLASCO C3 camera'sfield of view on 12 January,[11] and was viewable on theweb in near real-time. The comet left SOHO's field of view on 16 January.[11] Due to its proximity to the Sun, the Northern Hemisphere ground-based viewers had a short window for viewing, and the comet could be spotted only during bright twilight.[citation needed]
As it reached perihelion on 12 January, it became the brightest comet sinceComet Ikeya–Seki in 1965.[6] The comet was dubbed theGreat Comet of 2007 by Space.com.[12] On 13 and 14 January 2007, the comet attained an estimated maximumapparent magnitude of −5.5.[13] It was bright enough to be visible in daylight about 5°–10° southeast of the Sun from 12 to 14 January.[14] The closest approach to the Earth occurred on 15 January 2007, at a distance of 0.82 AU.[15]
After passing the Sun, McNaught became visible in the Southern Hemisphere. In Australia, according toSiding Spring Observatory atCoonabarabran, where the comet was discovered, it was to have reached its theoretical peak in brightness on Sunday 14 January just after sunset,[16] when it would have been visible for 23 minutes. On 15 January the comet was observed atPerth Observatory with an estimatedapparent magnitude of −4.0.[17][better source needed]
TheUlysses spacecraft made an unexpected pass through the tail of the comet on 3 February 2007.[18] Evidence of the encounter was published in the 1 October 2007 issue ofThe Astrophysical Journal.[19]Ulysses flew through McNaught's ion tail 260 million km (1.7 AU) from the comet's core and instrument readings showed that there was "complex chemistry" in the region.[18]
The Solar Wind Ion Composition Spectrometer (SWICS) aboardUlysses measured Comet McNaught's tail composition and detected unexpected ions. It was the first time that O3+ oxygen ions were detected near a comet. This suggested that the solar wind ions, which did not originally have most of their electrons, gained some electrons while passing through the comet's atmosphere.[18]
SWICS also measured the speed of thesolar wind, and found that even at 260 million kilometres (160 million miles) from the comet's nucleus, the tail had slowed the solar wind to half its normal speed. The solar wind should usually be about 700 km (430 mi) per second at that distance from the Sun, but inside the comet's ion tail, it was less than 401 km (249 mi) per second.[18]
This was very surprising to me. Way past the orbit of Mars, the solar wind felt the disturbance of this little comet. It will be a serious challenge for us theoreticians and computer modellers to figure out the physics
— Michael Combi,[18]
Prof. George Gloeckler, the principal investigator on the Solar Wind Ion Composition Spectrometer (SWICS), said the discovery was important as the composition of comets told them about conditions approximately 4.5 billion years ago when the Solar System was formed.
Here we got a direct sample of this ancient material which gives us the best information on cometary composition. We're still in the process of figuring out what it tells us. We're contributing part of the whole puzzle. The benefits of such an observation are important. They constrain the interactions of such comets with the Sun, including how the comets lose mass. They also examine the question of how a sudden injection of neutral and cold material interacts with hot solar-like plasmas. That occurs in other places of the universe and we were able to study it right here
Comet C/2006 P1 took millions of years coming directly from theOort cloud.[2] It follows ahyperbolic trajectory (with anosculating eccentricity larger than 1)[3] during its passage through the innerSolar System, but the eccentricity will drop below 1 after it leaves the influence of the planets and it will remain bound to the Solar System as an Oort cloud comet.[20]
Given theorbital eccentricity of this object, differentepochs can generate quite different heliocentric unperturbedtwo-bodybest-fit solutions to the aphelion distance (maximum distance) of this object.[b] For objects at such high eccentricity, the Sun'sbarycentric coordinates are more stable than heliocentric coordinates. UsingJPL Horizons, the barycentric orbital elements for epoch 2050 generate asemi-major axis of 2050 AU and a period of approximately 92,700 years.[21]
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