A Comet tail and coma are illuminated by the Sun and may become visible from Earth when a comet passes through the inner solar system, the dust reflecting sunlight directly and the gases glowing from ionisation. Most comets are too faint to be visible without the aid of a telescope, but a few each decade become bright enough to be visible to the naked eye.
The streams of dust and gas each form their own distinct tail, pointing in slightly different directions. The tail of dust is left behind in the comet's orbit in such a manner that it often forms a curved tail called the antitail. At the same time, the ion tail, made of gases, always points directly away from the Sun, as this gas is more strongly affected by the solar wind than is dust, following magnetic field lines rather than an orbital trajectory. Parallax viewing from the Earth may sometimes mean the tails appear to point in opposite directions.
While the solid nucleus of comets is generally less than 50 km across, the coma may be larger than the Sun, and ion tails have been observed to extend 1 astronomical unit (150 million km) or more. The observation of antitails contributed significantly to the discovery of solar wind. The ion tail is formed as a result of the photoelectric effect[dubious ] of solar ultra-violet radiation acting on particles in the coma. Once the particles have been ionised, they attain a net positive electrical charge which in turn gives rise to an "induced magnetosphere" around the comet. The comet and its induced magnetic field form an obstacle to outward flowing solar wind particles. As the relative orbital speed of the comet and the solar wind is supersonic a bow shock is formed upstream of the comet, in the flow direction of the solar wind. In this bow shock, large concentrations of cometary ions (called "pick-up ions") congregate and act to "load" the solar magnetic field with plasma, such that the field lines "drape" around the comet forming the ion tail.
Tail formation Edit
In the outer solar system, comets remain frozen and are extremely difficult or impossible to detect from Earth due to their small size. Statistical detections of inactive comet nuclei in the Kuiper belt have been reported from the Hubble Space Telescope observations, but these detections have been questioned, and have not yet been independently confirmed. As a comet approaches the inner solar system, solar radiation causes the volatile materials within the comet to vaporize and stream out of the nucleus, carrying dust away with them. The streams of dust and gas thus released form a huge, extremely tenuous atmosphere around the comet called the coma, and the force exerted on the coma by the Sun's radiation pressure and solar wind cause an enormous tail to form, which points away from the sun.
Tail loss Edit
If the ion tail loading is sufficient, then the magnetic field lines are squeezed together to the point where, at some distance along the ion tail, magnetic reconnection occurs. This leads to a "tail disconnection event". This has been observed on a number of occasions, notable among which was on the 20th. April 2007 when the ion tail of comet Encke was completely severed as the comet passed through a coronal mass ejection. This event was observed by the STEREO spacecraft.
Comets were found to emit X-rays in 1996. This surprised researchers, because X-ray emission is usually associated with very high-temperature bodies. The X-rays are thought to be generated by the interaction between comets and the solar wind: when highly charged ions fly through a cometary atmosphere, they collide with cometary atoms and molecules, "ripping of" one or more electrons from the comet. This ripping off leads to the emission of X-rays and far ultraviolet photons.
- ↑ McKenna, M. (20 May 2008). "Chasing an Anti-Tail". Astronomy Sketch of the Day. Retrieved on 2009-02-25.
- ↑ Yeomans, Donald K. (2005). "Comet". World Book Online Reference Center. World Book. Retrieved on 2008-12-27.
- ↑ Biermann, L. (1963). "The plasma tails of comets and the interplanetary plasma". Space Science Reviews 1 (3): 553. doi:10.1007/BF00225271.
- ↑ 4.0 4.1 Carroll, B. W.; Ostlie, D. A. (1996). An Introduction to Modern Astrophysics, Addison-Wesley. p. 864-874. ISBN 0201547309.
- ↑ Cochran, A. L.; Levison, H. F.; Stern, S. A.; Duncan, J. (1995). "The Discovery of Halley-sized Kuiper Belt Objects Using the Hubble Space Telescope". Astrophysical Journal 455: 342. doi:10.1086/176581. arΧiv:astro-ph/9509100, http://articles.adsabs.harvard.edu/full/1995ApJ...455..342C.
- ↑ Cochran, A. L.; Levison, H. F.; Tamblyn, P.; Stern, S. A.; Duncan, J. (1998). "The Calibration of the Hubble Space Telescope Kuiper Belt Object Search: Setting the Record Straight". Astrophysical Journal Letters 503 (1): L89. doi:10.1086/311515.
- ↑ Brown, Michael E.; Kulkarni, S. R.; Liggett, T. J. (1997). "An Analysis of the Statistics of the Hubble Space Telescope Kuiper Belt Object Search". Astrophysical Journal Letters 490 (1): L119. doi:10.1086/311009.
- ↑ Jewitt, David C.; Luu, Jane; Chen, J. (1996). "The Mauna Kea-Cerro-Tololo (MKCT) Kuiper Belt and Centaur Survey". Astronomical Journal 112 (3): 1225. doi:10.1086/118093, http://articles.adsabs.harvard.edu/full/1996AJ....112.1225J.
- ↑ Eyles, C. J.; Harrison, R. A.; Davis, C. J.; Waltham, N. R.; Shaughnessy, B. M.; Mapson-Menard, H. C. A.; Bewsher, D.; Crothers, S. R.; et al. (2009). "The Heliospheric Imagers Onboard the STEREO Mission". Solar Physics 254 (2): 387–445. doi:10.1007/s11207-008-9299-0.
- ↑ "First X-Rays from a Comet Discovered". Goddard Spaceflight Center. Retrieved on 2006-03-05.
- ↑ "Interaction model – Probing space weather with comets". KVI atomics physics. Archived from the original on 2006-02-13. Retrieved on 2009-04-26.
- Comets at the Open Directory Project
- Comets Page at NASA's Solar System Exploration
- Source of useful comet-related material on the Web