Udarni krater

Udarni krater Tycho na Mjesecu.

Udarni krater je jedan od najčešćih tipova kratera koji se spominju u astronomiji.

U najširem smislu, pojam udarni krater može se primijeniti na bilo koju depresiju, prirodnu ili izazvanu ljudskim utjecajem, koja proizilazi iz sudara (velike brzine) manjeg tijela s većim tijelom. Navedeni termin se najčešće koristi za kružne depresije na površini planeta, satelita ili drugih čvrstih tijela u Sunčevom sistemu, formirane od udara manjih tijela s podlogom. Za razliku od vulkanskih kratera, koji su rezultat eksplozije ili unutrašnjeg kolapsa,[1] ovi krateri obično su oivičeni i imaju pod koji je niži od visine okolnog terena.[2] Kratere nalazimo u raznim oblicima i to u rasponu od: malih jednostavnih zdjela, do velikih, složenih, multi-prstenastih bazena. Meteor Crater je možda najpoznatiji primjer malog kratera na Zemlji.

Utjecaj krateri su dominantna reljefna forma na mnogim čvrstim objektima Sunčevog sistema, uključujući Mjesec, Merkur, Kalisto, Ganimed i većinu malih satelita i asteroida. Na drugim planetama i mjesecima na kojima su više aktivni geološki procesi, kao što su Zemlja, Venera, Mars, Evropa, Ija i Titan, vidljivi krateri su rjeđi jer nestaju po utjecajima erozije, zatrpani ili preobraženi tektonskim procesima tokom vremena.

U ranom Sunčevom sistemu, stopa kolizija nebeskih tijela je bila mnogo veća nego danas. Veliki multi-prstenasti udarni bazeni, prečnika od nekoliko stotina kilometara ili više, zadržao se na primjer na Merkuru i Mjesecu. Rekordan period intenzivnog bombardovanja u unutrašnjem Sunčevom sistemu, je završio prije oko 3,8 milijardi godina. Od tog vremena, stopa nastanka novih kratera na Zemlji je znatno niža, ali je ipak primjetna. Zemlju pogode jedan do tri udara, dovoljno velika da načine krater prečnika 20 km, u prosjeku svakih milion godina .[3][4] To znači da ne bi trebalo biti puno više relativno mladih kratera na planeti nego što je dosada otkriveno.

Iako su Zemljini aktivni površinski procesi brzo uništili "zapise" udara, dosada je identifikovano oko 170 kopnenih kratera.[5] Njihova veličina je u rasponu prečnika od nekoliko desetina metara do oko 300 km, a vremenskog su raspona od modernih (npr. Sikhote-Alin krater u Rusiji koji je nastao 1947) do starih više od dvije milijarde godina, iako je većina mlađa od 500 miliona godina, pošto stariji krateri "iščezavaju" pod uticajem geoloških procesa. Mogu su također selektivno naći u stabilnim regijama u unutrašnjosti kontinenata.[6] Malo podmorskih kratera je otkriveno zbog teškoća pri istraživanju morskog dna, brze stope promjene na dnu okeana, i subdukcije na dnu okeana u Zemljinoj unutrašnjosti zbog procesa tektonike ploča.

Udarne kratere se ne smije miješati s drugim sličnim reljefnim oblicima koji se u nekim slučajevima pojavljuju, uključujući i kaldere prstenaste nasipe.

Također pogledajte

Reference

  1. ^ Basaltic Volcanism Study Project. (1981). Basaltic Volcanism on the Terrestrial Planets; Pergamon Press, Inc: New York, p. 746. http://articles.adsabs.harvard.edu//full/book/bvtp./1981//0000746.000.html.
  2. ^ Consolmagno, G.J.; Schaefer, M.W. (1994). Worlds Apart: A Textbook in Planetary Sciences; Prentice Hall: Englewood Cliffs, NJ, p.56.
  3. ^ Carr, M.H. (2006) The surface of Mars; Cambridge University Press: Cambridge, UK, p. 23.
  4. ^ Grieve R.A.; Shoemaker, E.M. (1994). The Record of Past Impacts on Earth in Hazards due to Comets and Asteroids, T. Gehrels, Ed.; University of Arizona Press, Tucson, AZ, pp. 417-464.
  5. ^ Grieve, R.A.F.; Cintala, M.J.; Tagle, R. (2007). Planetary Impacts in Encyclopedia of the Solar System, 2nd ed., L-A. McFadden et al. Eds, p. 826.
  6. ^ Shoemaker, E.M.; Shoemaker, C.S. (1999). The Role of Collisions in The New Solar System, 4th ed., J.K. Beatty et al., Eds., p. 73.


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