Editing Chicxulub crater (section)

===Impact rocks===
The most common observed [[impactite|impact rocks]] are [[suevite]]s, found in many of the boreholes drilled around the Chicxulub crater. Most of the suevites were resedimented soon after the impact by the resurgence of oceanic water into the crater. This gave rise to a layer of suevite extending from the inner part of the crater out as far as the outer rim.<ref name="Kaskes_etal_2022">{{Cite journal |last1=Kaskes |first1=P. |last2=de Graaf |first2=S.J. |last3=Feignon |first3=J.-G. |last4=Déhais |first4=T. |last5=Goderis |first5=S. |last6=Ferrière |first6=LO. |last7=Koeberl |first7=C. |last8=Smit |first8=J. |last9=Wittmann |first9=A. |last10=Gulick |first10=S.P.S. |last11=Debaille |first11=V. |last12=Mattielli|first12=N.|last13=Claeys|first13=P.|display-authors=3|year=2022 |title=Formation of the crater suevite sequence from the Chicxulub peak ring: A petrographic, geochemical, and sedimentological characterization |journal=GSA Bulletin |volume=134 |issue=3–4 |pages=895–927 |doi=10.1130/B36020.1|bibcode=2022GSAB..134..895K |s2cid=237762081|url=https://biblio.vub.ac.be/vubirfiles/72890608/b36020.pdf }}</ref>

Impact melt rocks are thought to fill the central part of the crater, with a maximum thickness of {{convert|3|km|sp=us}}. The samples of melt rock that have been studied have overall compositions similar to that of the basement rocks, with some indications of mixing with carbonate source, presumed to be derived from the Cretaceous carbonates. An analysis of melt rocks sampled by the M0077A borehole indicates two types of melt rock, an upper impact melt (UIM), which has a clear carbonate component as shown by its overall chemistry and the presence of rare limestone clasts and a lower impact melt-bearing unit (LIMB) that lacks any carbonate component. The difference between the two impact melts is interpreted to be a result of the upper part of the initial impact melt, represented by the LIMB in the borehole, becoming mixed with materials from the shallow part of the crust either falling back into the crater or being brought back by the resurgence forming the UIM.<ref name="de Graaf_etal_2022">{{Cite journal |last1=de Graaf |first1=S.J. |last2=Kaskes |first2=P. |last3=Déhais |first3=T. |last4=Goderis |first4=S. |last5=Debaille |first5=V. |last6=Ross |first6=C.H. |last7=Gulick |first7=S.P.S. |last8=Feignon |first8=J.-G. |last9=Ferrière |first9=L. |last10=Koeberi |first10=C. |last11=Smit |first11=J. |last12=Mattielli |first12=N. |last13=Claeys |first13=P. |display-authors=3 |year=2022 |title=New insights into the formation and emplacement of impact melt rocks within the Chicxulub impact structure, following the 2016 IODP-ICDP Expedition 364 |journal=GSA Bulletin |volume=134 |issue=1–2 |pages=293–315 |doi=10.1130/B35795.1 |bibcode=2022GSAB..134..293D |s2cid=236541913 |url=https://biblio.vub.ac.be/vubirfiles/79061460/deGraaff_ImpactMelt_GSA_B_Manuscript_v3_MasterFile_Clean.pdf |access-date=May 18, 2022 |archive-date=May 18, 2022 |archive-url=https://web.archive.org/web/20220518033352/https://biblio.vub.ac.be/vubirfiles/79061460/deGraaff_ImpactMelt_GSA_B_Manuscript_v3_MasterFile_Clean.pdf |url-status=live }}</ref>

The "pink granite", a granitoid rich in [[alkali feldspar]] found in the peak ring borehole shows many deformation features that record the extreme strains associated with the formation of the crater and the subsequent development of the peak ring.<ref name="Kring_2017" /><ref>{{cite news|last1=St. Fleur|first1=Nicholas|title=Drilling into the Chicxulub Crater, Ground Zero of the Dinosaur Extinction|url=https://www.nytimes.com/2016/11/18/science/chicxulub-crater-dinosaur-extinction.html|newspaper=The New York Times|date=November 17, 2016|access-date=March 1, 2017|archive-date=November 19, 2016|archive-url=https://web.archive.org/web/20161119200501/http://www.nytimes.com/2016/11/18/science/chicxulub-crater-dinosaur-extinction.html?_r=0|url-status=live}}</ref> The granitoid has an unusually low density and [[P-wave]] velocity compared to typical granitic basement rocks. Study of the core from M0077A shows the following deformation features in apparent order of development: pervasive fracturing along and through grain boundaries, a high density of [[shear fault]]s, bands of [[cataclasite]] and ultra-cataclasite and some [[shear zone|ductile shear structures]]. This deformation sequence is interpreted to result from initial crater formation involving [[acoustic fluidization]] followed by shear faulting with the development of cataclasites with [[fault zone]]s containing impact melts.<ref name="Riller_etal_2018">{{Cite journal |last1=Riller |first1=U. |last2=Poelchau |first2=M.H. |last3=Rae |first3=A.S.P. |last4=Schulte |first4=F.M. |last5=Collins |first5=G.S. |last6=Melish |first6=H.J. |last7=Grieve |first7=R.A.F. |last8=Morgan |first8=J.V.|author8-link= Joanna Morgan |last9=Gulick |first9=S.P. |last10=Lofi |first10=J. |last11=Diaw |first11=A. |last12=McCall|first12=N.|last13=Kring|first13=D.A.|last14=((IODP–ICDP Expedition 364 Science Party))|display-authors=3|year=2018 |title=Rock fluidization during peak-ring formation of large impact structures |journal=Nature |volume=562 |issue=7728 |pages=511–518 |doi=10.1038/s41586-018-0607-z|pmid=30356184 |bibcode=2018Natur.562..511R |s2cid=53026325|url=http://eprints.gla.ac.uk/173925/1/173925.pdf }}</ref>

The peak ring drilling below the sea floor also discovered evidence of a massive hydrothermal system, which modified approximately {{nowrap|1.4 × 10<sup>5</sup> km<sup>3</sup>}} of Earth's crust and lasted for hundreds of thousands of years. These hydrothermal systems may provide support for the impact origin of life hypothesis for the [[Hadean]] eon,<ref>{{cite journal<!--|authors=David A. Kring; Sonia M. Tikoo; Martin Schmieder1; Ulrich Riller; Mario Rebolledo-Vieyra; Sarah L. Simpson; Gordon R. Osinski; Jérôme Gattacceca; Axel Wittmann; Christina M. Verhagen; Charles S. Cockell; Marco J.L. Coolen; Fred J. Longstaffe; Sean P. S. Gulick; [[Joanna Morgan|Joanna V. Morgan]]; Timothy J. Bralower; Elise Chenot; Gail L. Christeson; Philippe Claeys; Ludovic Ferrière; Catalina Gebhardt; Kazuhisa Goto; Sophie L. Green; Heather Jones; Johanna Lofi; Christopher M. Lowery; Rubén Ocampo-Torres; Ligia Perez-Cruz; Annemarie E. Pickersgill; Michael H. Poelchau; Auriol S.P. Rae11; Cornelia Rasmussen; Honami Sato; Jan Smit; Naotaka Tomioka; Jaime Urrutia-Fucugauchi; Michael T. Whalen; Long Xiao and Kosei E. Yamaguchi-->|last1=Kring |first1=David |first2=Sonia M. |last2=Tikoo |first3=Martin |last3=Schmieder |display-authors=etal|title=Probing the hydrothermal system of the Chicxulub impact crater|journal=Science Advances |year=2020|volume=6|issue=22|doi=10.1126/sciadv.aaz3053|s2cid=219244669}}</ref> when the entire surface of Earth was affected by impactors much larger than the Chicxulub impactor.<ref>{{cite journal |first2= W.F. |last2=Bottke |first3=L.T. |last3=Elkins-Tanton |first4=M. |last4=Bierhaus|first5= K. |last5=Wuennemann|first6=A. |last6=Morbidelli |first7=D.A. |last7=Kring|last1=Marchi |first1=S. |display-authors=3|title=Widespread mixing and burial of Earth's Hadean crust by asteroid impacts|journal=Nature|year=2014|volume=511|issue=7511 |pages=578–582|doi=10.1038/nature13539|pmid=25079556 |bibcode=2014Natur.511..578M |s2cid=205239647}}</ref>