Editing 7 Iris (section)

===Geology===
Iris is an S-type asteroid. The surface is bright and is probably a mixture of [[nickel]]-[[iron]] metals and [[magnesium]]- and iron-[[silicate]]s. Its spectrum is similar to that of [[L chondrite|L]] and [[LL chondrite]]s with corrections for [[space weathering]],<ref name="Ueda2003">{{Cite conference |last1=Ueda |first1=Y. |last2=Miyamoto |first2=M. |last3=Mikouchi |first3=T. |last4=Hiroi |first4=T. |date=March 2003 |title=Surface Material Analysis of the S-type Asteroids: Removing the Space Weathering Effect from Reflectance Spectrum |conference=34th Annual Lunar and Planetary Science Conference |pages=2078 |bibcode=2003LPI....34.2078U}}</ref> so it may be an important  contributor of these [[meteorites]]. Planetary dynamics also indicates that it should be a significant source of meteorites.<ref name="Migliorini">{{cite journal| bibcode=1997A&A...321..652M| first1= F.|last1= Migliorini| title=(7) Iris: a possible source of ordinary chondrites?| journal=Astronomy & Astrophysics| volume= 321| pages=652| date=1997| first2=A.|last2=Manara|first3=A.| last3=Cellino|first4=M.| last4=Di Martino|first5=V.| last5=Zappala|display-authors=1}}
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Among the [[S-type asteroid]]s, Iris ranks fifth in [[mean diameter]] after [[15 Eunomia|Eunomia]], [[3 Juno|Juno]], [[29 Amphitrite|Amphitrite]] and [[532 Herculina|Herculina]]. Its shape is consistent with an oblate spheroid with a large equatorial excavation, suggesting it is a remnant planetesimal. No collisional family can be associated with Iris, likely because the excavating impact occurred early in the history of the Solar System, and the debris has since dispersed.<ref name="Hanus2019"/>