Editing Basalt (section)

====Io====
Lava flows represent a major volcanic terrain on [[Io (moon)|Io]].<ref name="Keszthelyi2001">{{cite journal |last1=Keszthelyi |first1=L. |last2=McEwen |first2=A. S. |last3=Phillips |first3=C. B.|author3-link=Cynthia B. Phillips |last4=Milazzo |first4=M. |last5=Geissler |first5=P. |last6=Turtle |first6=E. P. |last7=Radebaugh |first7=J. |last8=Williams |first8=D. A. |last9=Simonelli |first9=D. P. |last10=Breneman |first10=H. H. |last11=Klaasen |first11=K. P. |last12=Levanas |first12=G. |last13=Denk |first13=T. |title=Imaging of volcanic activity on Jupiter's moon Io by Galileo during the Galileo Europa Mission and the Galileo Millennium Mission |journal=Journal of Geophysical Research: Planets |date=2001-12-25 |volume=106 |issue=E12 |pages=33025–33052 |doi=10.1029/2000JE001383 |bibcode=2001JGR...10633025K |doi-access=free }}</ref> Analysis of the ''Voyager'' images led scientists to believe that these flows were composed mostly of various compounds of molten sulfur. However, subsequent Earth-based [[infrared]] studies and measurements from the ''Galileo'' spacecraft indicate that these flows are composed of basaltic lava with mafic to ultramafic compositions.<ref name="Battaglia2019">{{Cite conference |title= A Jökulhlaup-like Model for Secondary Sulfur Flows on Io |conference=50th Lunar and Planetary Science Conference. 18–22 March 2019. The Woodlands, Texas. |first=Steven M. |last=Battaglia |date=March 2019 |id=LPI Contribution No. 1189 |url=https://www.hou.usra.edu/meetings/lpsc2019/pdf/1189.pdf | bibcode=2019LPI....50.1189B}}</ref> This conclusion is based on temperature measurements of Io's "hotspots", or thermal-emission locations, which suggest temperatures of at least 1,300&nbsp;K and some as high as 1,600&nbsp;K.<ref name="Keszthelyi2007">{{cite journal |last1=Keszthelyi |first1=Laszlo |last2=Jaeger |first2=Windy |last3=Milazzo |first3=Moses |last4=Radebaugh |first4=Jani |last5=Davies |first5=Ashley Gerard |last6=Mitchell |first6=Karl L. |title=New estimates for Io eruption temperatures: Implications for the interior |journal=Icarus |date=December 2007 |volume=192 |issue=2 |pages=491–502 |doi=10.1016/j.icarus.2007.07.008 |bibcode=2007Icar..192..491K |url=https://zenodo.org/record/1259031 }}</ref> Initial estimates suggesting eruption temperatures approaching 2,000&nbsp;K<ref name="Mcewen1998b">{{cite journal |title=High-temperature silicate volcanism on Jupiter's moon Io |journal=Science |last=McEwen |first=A. S. |display-authors=etal |pages=87–90 |volume=281 |issue=5373 |date=1998 |doi=10.1126/science.281.5373.87 |pmid=9651251 |bibcode=1998Sci...281...87M |s2cid=28222050 }}</ref> have since proven to be overestimates because the wrong thermal models were used to model the temperatures.<ref name="Keszthelyi2007"/>{{sfn|Battaglia|2019}}