Meteor shower

Last updated on 2 October 2017

A meteor shower is a celestial event in which a number of meteors are observed to radiate, or originate, from one point in the night sky. These meteors are caused by streams of cosmic debris called meteoroids entering Earth's atmosphere at extremely high speeds on parallel trajectories. Most meteors are smaller than a grain of sand, so almost all of them disintegrate and never hit the Earth's surface. Intense or unusual meteor showers are known as meteor outbursts and meteor storms, which may produce greater than 1000 meteors an hour.[1] The Meteor Data Centre lists about 600 suspected meteor showers of which about 100 are well established.[2]

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Four-hour time lapse exposure of the sky
Leonid meteor shower as seen from space (1997).jpg
Leonids from space

Historical developments

PSM V01 D405 August meteor shower orbit.jpg
Diagram from 1872

The first great storm in the modern era was the Leonids of November 1833. One estimate is over one hundred thousand meteors an hour,[3] but another, done as the storm abated, estimated in excess of two hundred thousand meteors during the 9 hours of storm[4] over the entire region of North America east of the Rocky Mountains. American Denison Olmsted (1791−1859) explained the event most accurately. After spending the last weeks of 1833 collecting information he presented his findings in January 1834 to the American Journal of Science and Arts, published in January–April 1834,[5] and January 1836.[6] He noted the shower was of short duration and was not seen in Europe, and that the meteors radiated from a point in the constellation of Leo and he speculated the meteors had originated from a cloud of particles in space.[7] Work continued, yet coming to understand the annual nature of showers though the occurrences of storms perplexed researchers.[8]

In the 1890s, Irish astronomer George Johnstone Stoney (1826–1911) and British astronomer Arthur Matthew Weld Downing (1850–1917), were the first to attempt to calculate the position of the dust at Earth's orbit. They studied the dust ejected in 1866 by comet 55P/Tempel-Tuttle in advance of the anticipated Leonid shower return of 1898 and 1899. Meteor storms were anticipated, but the final calculations showed that most of the dust would be far inside of Earth's orbit. The same results were independently arrived at by Adolf Berberich of the Königliches Astronomisches Rechen Institut (Royal Astronomical Computation Institute) in Berlin, Germany. Although the absence of meteor storms that season confirmed the calculations, the advance of much better computing tools was needed to arrive at reliable predictions.

In 1981 Donald K. Yeomans of the Jet Propulsion Laboratory reviewed the history of meteor showers for the Leonids and the history of the dynamic orbit of Comet Tempel-Tuttle.[9] A graph [10] from it was adapted and re-published in Sky and Telescope.[11] It showed relative positions of the Earth and Tempel-Tuttle and marks where Earth encountered dense dust. This showed that the meteoroids are mostly behind and outside the path of the comet, but paths of the Earth through the cloud of particles resulting in powerful storms were very near paths of nearly no activity.

In 1985, E. D. Kondrat'eva and E. A. Reznikov of Kazan State University first correctly identified the years when dust was released which was responsible for several past Leonid meteor storms. In 1995, Peter Jenniskens predicted the 1995 Alpha Monocerotids outburst from dust trails.[12] In anticipation of the 1999 Leonid storm, Robert H. McNaught,[13] David Asher,[14] and Finland's Esko Lyytinen were the first to apply this method in the West.[15][16] In 2006 Jenniskens has published predictions for future dust trail encounters covering the next 50 years.[17] Jérémie Vaubaillon continues to update predictions based on observartions each year for the Institut de Mécanique Céleste et de Calcul des Éphémérides (IMCCE).[18]

Radiant point

PSM V18 D201 Shower of perseids sept 6 and 7.jpg
Meteor shower on chart

Because meteor shower particles are all traveling in parallel paths, and at the same velocity, they will all appear to an observer below to radiate away from a single point in the sky. This radiant point is caused by the effect of perspective, similar to parallel railroad tracks converging at a single vanishing point on the horizon when viewed from the middle of the tracks. Meteor showers are almost always named after the constellation from which the meteors appear to originate. This "fixed point" slowly moves across the sky during the night due to the Earth turning on its axis, the same reason the stars appear to slowly march across the sky. The radiant also moves slightly from night to night against the background stars (radiant drift) due to the Earth moving in its orbit around the sun. See IMO Meteor Shower Calendar 2017 (International Meteor Organization) for maps of drifting "fixed points."

When the moving radiant is at the highest point it will reach in the observer's sky that night, the sun will be just clearing the eastern horizon. For this reason, the best viewing time for a meteor shower is generally slightly before dawn — a compromise between the maximum number of meteors available for viewing, and the lightening sky which makes them harder to see.


Meteor showers are named after the nearest constellation or bright star with a Greek or Roman letter assigned that is close to the radiant position at the peak of the shower, whereby the grammatical declension of the Latin possessive form is replaced by "id" or "ids". Hence, meteors radiating from near the star delta Aquarii (declension "-i") are called delta Aquariids. The International Astronomical Union's Task Group on Meteor Shower Nomenclature and the IAU's Meteor Data Center keep track of meteor shower nomenclature and which showers are established.

Origin of meteoroid streams

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Comet Encke's meteoroid trail is the diagonal red glow
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Meteoroid trail between fragments of Comet 73P

A meteor shower is the result of an interaction between a planet, such as Earth, and streams of debris from a comet. Comets can produce debris by water vapor drag, as demonstrated by Fred Whipple in 1951,[19] and by breakup. Whipple envisioned comets as "dirty snowballs," made up of rock embedded in ice, orbiting the Sun. The "ice" may be water, methane, ammonia, or other volatiles, alone or in combination. The "rock" may vary in size from that of a dust mote to that of a small boulder. Dust mote sized solids are orders of magnitude more common than those the size of sand grains, which, in turn, are similarly more common than those the size of pebbles, and so on. When the ice warms and sublimates, the vapor can drag along dust, sand, and pebbles.

Each time a comet swings by the Sun in its orbit, some of its ice vaporizes and a certain amount of meteoroids will be shed. The meteoroids spread out along the entire orbit of the comet to form a meteoroid stream, also known as a "dust trail" (as opposed to a comet's "dust tail" caused by the very small particles that are quickly blown away by solar radiation pressure).

Recently, Peter Jenniskens[17] has argued that most of our short-period meteor showers are not from the normal water vapor drag of active comets, but the product of infrequent disintegrations, when large chunks break off a mostly dormant comet. Examples are the Quadrantids and Geminids, which originated from a breakup of asteroid-looking objects, 2003 EH1 and 3200 Phaethon, respectively, about 500 and 1000 years ago. The fragments tend to fall apart quickly into dust, sand, and pebbles, and spread out along the orbit of the comet to form a dense meteoroid stream, which subsequently evolves into Earth's path.

Dynamical evolution of meteoroid streams

Shortly after Whipple predicted that dust particles travelled at low speeds relative to the comet, Milos Plavec was the first to offer the idea of a dust trail, when he calculated how meteoroids, once freed from the comet, would drift mostly in front of or behind the comet after completing one orbit. The effect is simple orbital mechanics – the material drifts only a little laterally away from the comet while drifting ahead or behind the comet because some particles make a wider orbit than others.[17] These dust trails are sometimes observed in comet images taken at mid infrared wavelengths (heat radiation), where dust particles from the previous return to the Sun are spread along the orbit of the comet (see figures).

The gravitational pull of the planets determines where the dust trail would pass by Earth orbit, much like a gardener directing a hose to water a distant plant. Most years, those trails would miss the Earth altogether, but in some years the Earth is showered by meteors. This effect was first demonstrated from observations of the 1995 alpha Monocerotids,[20][21] and from earlier not widely known identifications of past earth storms.

Over longer periods of time, the dust trails can evolve in complicated ways. For example, the orbits of some repeating comets, and meteoroids leaving them, are in resonant orbits with Jupiter or one of the other large planets – so many revolutions of one will equal another number of revolutions of the other. This creates a shower component called a filament.

A second effect is a close encounter with a planet. When the meteoroids pass by Earth, some are accelerated (making wider orbits around the Sun), others are decelerated (making shorter orbits), resulting in gaps in the dust trail in the next return (like opening a curtain, with grains piling up at the beginning and end of the gap). Also, Jupiter's perturbation can change sections of the dust trail dramatically, especially for short period comets, when the grains approach the big planet at their furthest point along the orbit around the Sun, moving most slowly. As a result, the trail has a clumping, a braiding or a tangling of crescents, of each individual release of material.

The third effect is that of radiation pressure which will push less massive particles into orbits further from the sun – while more massive objects (responsible for bolides or fireballs) will tend to be affected less by radiation pressure. This makes some dust trail encounters rich in bright meteors, others rich in faint meteors. Over time, these effects disperse the meteoroids and create a broader stream. The meteors we see from these streams are part of annual showers, because Earth encounters those streams every year at much the same rate.

When the meteoroids collide with other meteoroids in the zodiacal cloud, they lose their stream association and become part of the "sporadic meteors" background. Long since dispersed from any stream or trail, they form isolated meteors, not a part of any shower. These random meteors will not appear to come from the radiant of the main shower.

Famous meteor showers

Perseids and Leonids

The most visible meteor shower in most years are the Perseids, which peak on 12 August of each year at over one meteor per minute. NASA has a useful tool to calculate how many meteors per hour are visible from one's observing location.

The Leonid meteor shower peaks around 17 November of each year. Approximately every 33 years, the Leonid shower produces a meteor storm, peaking at rates of thousands of meteors per hour. Leonid storms gave birth to the term meteor shower when it was first realised that, during the November 1833 storm, the meteors radiated from near the star Gamma Leonis. The last Leonid storms were in 1999, 2001 (two), and 2002 (two). Before that, there were storms in 1767, 1799, 1833, 1866, 1867, and 1966. When the Leonid shower is not storming, it is less active than the Perseids.

Other meteor showers

Established meteor showers

Official names are given in the International Astronomical Union's list of meteor showers.[22]

Shower Time Parent object
Quadrantids early January The same as the parent object of minor planet 2003 EH1,[23] and Comet C/1490 Y1.[24][25] Comet C/1385 U1 has also been studied as a possible source [26]
Lyrids late April Comet Thatcher
Pi Puppids (periodic) late April Comet 26P/Grigg-Skjellerup
Eta Aquariids early May Comet 1P/Halley
Arietids mid-June Comet 96P/Machholz, Marsden and Kracht comet groups complex [1][27]
June Bootids (periodic) late June Comet 7P/Pons-Winnecke
Southern Delta Aquariids late July Comet 96P/Machholz, Marsden and Kracht comet groups complex [1][27]
Alpha Capricornids late July Comet 169P/NEAT[28]
Perseids mid-August Comet 109P/Swift-Tuttle
Kappa Cygnids mid-August Minor planet 2008 ED69[29]
Aurigids (periodic) early September Comet C/1911 N1 (Kiess)[30]
Draconids (periodic) early October Comet 21P/Giacobini-Zinner
Orionids late October Comet 1P/Halley
Southern Taurids early November Comet 2P/Encke
Northern Taurids mid-November Minor planet 2004 TG10 and others[1][31]
Andromedids (periodic) mid-November Comet 3D/Biela[32]
Alpha Monocerotids (periodic) mid-November unknown[33]
Leonids mid-November Comet 55P/Tempel-Tuttle
Phoenicids (periodic) early December Comet 289P/Blanpain[34]
Geminids mid-December Minor planet 3200 Phaethon[35]
Ursids late December Comet 8P/Tuttle[36]

Extraterrestrial meteor showers

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Mars meteor by MER Spirit rover

Any other solar system body with a reasonably transparent atmosphere can also have meteor showers. As the Moon is in the neighborhood of Earth it can experience the same showers, but will have its own phenomena due to its lack of an atmosphere per se, such as vastly increasing its sodium tail.[37] NASA now maintains an ongoing database of observed impacts on the moon.[38] maintained by the Marshall Space Flight Center whether from a shower or not.

Many planets and moons have impact craters dating back large spans of time. But new craters, perhaps even related to meteor showers are possible. Mars, and thus its moons, is known to have meteor showers.[39] These have not been observed on other planets as yet but may be presumed to exist. For Mars in particular, although these are different from the ones seen on Earth because the different orbits of Mars and Earth relative to the orbits of comets. The Martian atmosphere has less than one percent of the density of Earth's at ground level, at their upper edges, where meteoroids strike, the two are more similar. Because of the similar air pressure at altitudes for meteors, the effects are much the same. Only the relatively slower motion of the meteoroids due to increased distance from the sun should marginally decrease meteor brightness. This is somewhat balanced in that the slower descent means that Martian meteors have more time in which to ablate.[40]

On March 7, 2004, the panoramic camera on Mars Exploration Rover Spirit recorded a streak which is now believed to have been caused by a meteor from a Martian meteor shower associated with comet 114P/Wiseman-Skiff. A strong display from this shower was expected on December 20, 2007. Other showers speculated about are a "Lambda Geminid" shower associated with the Eta Aquariids of Earth (i.e., both associated with Comet 1P/Halley), a "Beta Canis Major" shower associated with Comet 13P/Olbers, and "Draconids" from 5335 Damocles.[41]

Isolated massive impacts have been observed at Jupiter: The 1994 Comet Shoemaker–Levy 9 which formed a brief trail as well, and successive events since then (see List of Jupiter events.) Meteors or meteor showers have been discussed for most of the objects in the solar system with an atmosphere: Mercury,[42] Venus,[43] Saturn's moon Titan,[44] Neptune's moon Triton,[45] and Pluto.[46]

See also


  1. ^ a b c d Jenniskens, P. (2006). Meteor Showers and their Parent Comets. Cambridge University Press. ISBN 978-0-521-85349-1.
  2. ^ Meteor Data Center list of Meteor Showers
  3. ^ The 1833 Leonid Meteor Shower: A Frightening Flurry
  4. ^ Leonid MAC Brief history of the Leonid shower
  5. ^ Olmsted, Denison (1833). "Observations on the Meteors of November 13th, 1833". The American journal of science and arts. 25: 363–411. Retrieved 21 May 2013.
  6. ^ Olmsted, Denison (1836). "Facts respecting the Meteoric Phenomena of November 13th, 1834.". The American journal of science and arts. 29 (1): 168–170.
  7. ^ Observing the Leonids Gary W. Kronk
  8. ^ F.W. Russell, Meteor Watch Organizer, by Richard Taibi, May 19, 2013, accessed 21 May 2013
  9. ^ Yeomans, Donald K. (September 1981). "Comet Tempel-Tuttle and the Leonid meteors". Icarus. 47 (3): 492–499. Bibcode:1981Icar...47..492Y. doi:10.1016/0019-1035(81)90198-6{{inconsistent citations}}
  10. ^
  11. ^ Comet 55P/Tempel-Tuttle and the Leonid Meteors(1996, see p. 6)
  12. ^ Article published in 1997, notes prediction in 1995 - Jenniskens, P.; Betlem, H.; De Lignie, M.; Langbroek, M. (1997). "The Detection of a Dust Trail in the Orbit of an Earth-threatening Long-Period Comet". Astrophysical Journal. 479: 441. Bibcode:1997ApJ...479..441J. doi:10.1086/303853.
  13. ^ Re: (meteorobs) Leonid Storm? By Rob McNaught,
  14. ^ Blast from the Past Armagh Observatory press release 1999 April 21st.
  15. ^ Royal Astronomical Society Press Notice Ref. PN 99/27, Issued by: Dr Jacqueline Mitton RAS Press Officer
  16. ^ Voyage through a comet's trail, The 1998 Leonids sparkled over Canada By BBC Science's Dr Chris Riley on board NASA's Leonid mission
  17. ^ a b c Jenniskens P. (2006). Meteor Showers and their Parent Comets. Cambridge University Press, Cambridge, U.K., 790 pp.
  18. ^ IMCCE Prediction page Archived 2012-10-08 at the Wayback Machine.
  19. ^ Whipple, F. L. (1951). "A Comet Model. II. Physical Relations for Comets and Meteors". Astrophys. J. 113: 464. Bibcode:1951ApJ...113..464W. doi:10.1086/145416.
  20. ^ Jenniskens P., 1997. Meteor steram activity IV. Meteor outbursts ad the reflex motion of the Sun. Astron. Astrophys. 317, 953–961.
  21. ^ Jenniskens P., Betlem, H., De Lignie, M., Langbroek, M. (1997). The detection of a dust trail in the orbit of an Earth-threatening long-period comet. Astrohys. J. 479, 441–447.
  22. ^ "List of all meteor showers". International Astronomical Union. 15 August 2015.
  23. ^ Jenniskens, P. (March 2004). "2003 EH1 is the Quadrantid shower parent comet". Astronomical Journal. 127 (5): 3018–3022. Bibcode:2004AJ....127.3018J. doi:10.1086/383213.
  24. ^ Ball, Phillip. Dead comet spawned New Year meteors, Nature online website, ISSN 1744-7933, doi:10.1038/news031229-5, published online on December 31, 2003.
  25. ^ Haines, Lester, Meteor shower traced to 1490 comet break-up: Quadrantid mystery solved, The Register, January 8, 2008.
  26. ^ Marco Micheli; Fabrizio Bernardi; David J. Tholen (May 16, 2008). "Updated analysis of the dynamical relation between asteroid 2003 EH1 and comets C/1490 Y1 and C/1385 U1". Monthly Notices of the Royal Astronomical Society: Letters. 390 (1): L6–L8. Bibcode:2008MNRAS.390L...6M. arXiv:0805.2452Freely accessible. doi:10.1111/j.1745-3933.2008.00510.x.
  27. ^ a b Sekanina, Zdeněk; Chodas, Paul W. (December 2005). "Origin of the Marsden and Kracht Groups of Sunskirting Comets. I. Association with Comet 96P/Machholz and Its Interplanetary Complex". Astrophysical Journal Supplement Series. 161 (2): 551. Bibcode:2005ApJS..161..551S. doi:10.1086/497374.
  28. ^ Jenniskens, P.; Vaubaillon, J. (2010). "Minor Planet 2002 EX12 (=169P/NEAT) and the Alpha Capricornid Shower". Astronomical Journal. 139 (5): 1822–1830. Bibcode:2010AJ....139.1822J. doi:10.1088/0004-6256/139/5/1822.
  29. ^ Jenniskens, P.; Vaubaillon, J. (2008). "Minor Planet 2008 ED69 and the Kappa Cygnid Meteor Shower". Astronomical Journal. 136 (2): 725–730. Bibcode:2008AJ....136..725J. doi:10.1088/0004-6256/136/2/725.
  30. ^ Jenniskens, Peter; Vaubaillon, Jérémie (2007). "An Unusual Meteor Shower on 1 September 2007". Eos, Transactions, American Geophysical Union. 88 (32): 317–318. Bibcode:2007EOSTr..88..317J. doi:10.1029/2007EO320001.
  31. ^ Porubčan, V.; Kornoš, L.; Williams, I.P. (2006). "The Taurid complex meteor showers and asteroids". Contributions of the Astronomical Observatory Skalnaté Pleso. 36: 103–117. Bibcode:2006CoSka..36..103P. arXiv:0905.1639Freely accessible.
  32. ^ Jenniskens, P.; Vaubaillon, J. (2007). "3D/Biela and the Andromedids: Fragmenting versus Sublimating Comets". The Astronomical Journal. 134 (3): 1037. Bibcode:2007AJ....134.1037J. doi:10.1086/519074.
  33. ^ Jenniskens, P.; Betlem, H.; De Lignie, M.; Langbroek, M. (1997). "The Detection of a Dust Trail in the Orbit of an Earth-threatening Long-Period Comet". Astrophysical Journal. 479: 441. Bibcode:1997ApJ...479..441J. doi:10.1086/303853.
  34. ^ Jenniskens, P.; Lyytinen, E. (2005). "Meteor Showers from the Debris of Broken Comets: D/1819 W1 (Blanpain), 2003 WY25, and the Phoenicids". Astronomical Journal. 130 (3): 1286–1290. Bibcode:2005AJ....130.1286J. doi:10.1086/432469.
  35. ^ Brian G. Marsden (1983-10-25). "IAUC 3881: 1983 TB AND THE GEMINID METEORS; 1983 SA; KR Aur". International Astronomical Union Circular. Retrieved 2011-07-05.
  36. ^ Jenniskens, P.; Lyytinen, E.; De Lignie, M.C.; Johannink, C.; Jobse, K.; Schievink, R.; Langbroek, M.; Koop, M.; Gural, P.; Wilson, M.A.; Yrjölä, I.; Suzuki, K.; Ogawa, H.; De Groote, P. (2002). "Dust Trails of 8P/Tuttle and the Unusual Outbursts of the Ursid Shower". Icarus. 159: 197–209. Bibcode:2002Icar..159..197J. doi:10.1006/icar.2002.6855.
  37. ^ Hunten, D. M. (1991). "A possible meteor shower on the Moon". Geophysical Research Letters. 18: 2101–2104. Bibcode:1991GeoRL..18.2101H. doi:10.1029/91GL02543.
  38. ^ Lunar Impacts
  39. ^ Meteor showers at Mars
  40. ^ Can Meteors Exist at Mars?
  41. ^ Meteor Showers and their Parent Bodies
  42. ^ Rosemary M. Killen; Joseph M. Hahn (December 10, 2014). "Impact Vaporization as a Possible Source of Mercury’s Calcium Exosphere". Icarus. 250: 230–237. Bibcode:2015Icar..250..230K. doi:10.1016/j.icarus.2014.11.035. (Subscription required (help)).
  43. ^ The P/Halley Stream: Meteor Showers on Earth, Venus and Mars, by Apoistolos A. Christou, Geremie Vaubaillon and Paul Withers, Earth, Moon, and Planets, vol 102, # 1-4, doi:10.1007/s11038-007-9201-3
  44. ^ Lakdawalla, Emily. "Meteor showers on Titan: an example of why Twitter is awesome for scientists and the public". Retrieved 3 June 2013.
  45. ^ Watching meteors on Triton, W. Dean Pesnell, J.M. Grebowsky, and Andrew L. Weisman, Icarus, issue 169, (2004) pp. 482-491
  46. ^ IR Flashes induced by meteoroid impacts onto Pluto's surface, by I.B. Kosarev, I. V. Nemtchinov, Microsymposium, vol. 36, MS 050, 2002

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