Editing Comet (section)

===Bow shock===
[[Bow shock]]s form as a result of the interaction between the solar wind and the cometary ionosphere, which is created by the ionization of gases in the coma. As the comet approaches the Sun, increasing outgassing rates cause the coma to expand, and the sunlight ionizes gases in the coma. When the solar wind passes through this ion coma, the bow shock appears.

The first observations were made in the 1980s and 1990s as several spacecraft flew by comets [[21P/Giacobini–Zinner]],<ref>{{cite journal |title=The Bow wave of Comet Giacobini-Zinner – ICE magnetic field observations |journal=Geophysical Research Letters |last1=Jones |first1=D. E. |last2=Smith |first2=E. J. |last3=Slavin |first3=J. A. |last4=Tsurutani |first4=B. T. |last5=Siscoe |first5=G. L. |last6=Mendis |first6=D. A. |display-authors=1 |volume=13 |issue=3 |pages=243–246 |date=March 1986 |bibcode=1986GeoRL..13..243J |doi=10.1029/GL013i003p00243}}</ref> 1P/Halley,<ref>{{cite journal |title=First in situ plasma and neutral gas measurements at comet Halley |journal=Nature |first1=K. I.|last1=Gringauz|first2= T. I. |last2=Gombosi |first3=A. P. |last3=Remizov |first4=I. |last4=Apáthy |first5=I. |last5=Szemerey |first6=M. I. |last6=Verigin |first7=L. I. |last7=Denchikova |first8=A. V. |last8=Dyachkov |first9=E. |last9=Keppler |first10=I. N. |last10=Klimenko |first11=A. K. |last11=Richter |first12=A. J. |last12=Somogyi |first13=K. |last13=Szegő |first14=S. |last14=Szendrő |first15=M. |last15=Tátrallyay |first16=A. |last16=Varga |first17= G. A. |last17=Vladimirova |display-authors=1 |volume=321 |pages=282–285 |date=15 May 1986 |bibcode=1986Natur.321..282G |doi=10.1038/321282a0|s2cid=117920356 }}</ref> and [[26P/Grigg–Skjellerup]].<ref>{{cite journal |title=First results from the Giotto magnetometer experiment during the P/Grigg-Skjellerup encounter |journal=[[Astronomy & Astrophysics]] |first1=F. M. |last1=Neubauer |first2=H. |last2=Marschall |first3=M. |last3=Pohl |first4=K.-H. |last4=Glassmeier |first5=G. |last5=Musmann |first6=F. |last6=Mariani |first7=M. H. |last7=Acuna |first8=L. F. |last8=Burlaga |first9=N. F. |last9=Ness |first10=M. K. |last10=Wallis |first11=H. U. |last11=Schmidt |first12=E. |last12=Ungstrup |display-authors=1 |volume=268 |issue=2 |pages=L5–L8 |date=February 1993 |bibcode=1993A&A...268L...5N}}</ref> It was then found that the bow shocks at comets are wider and more gradual than the sharp planetary bow shocks seen at, for example, Earth. These observations were all made near [[perihelion]] when the bow shocks already were fully developed.

The [[Rosetta (spacecraft)|''Rosetta'']] spacecraft observed the bow shock at comet [[67P/Churyumov–Gerasimenko]] at an early stage of bow shock development when the outgassing increased during the comet's journey toward the Sun. This young bow shock was called the "infant bow shock". The infant bow shock is asymmetric and, relative to the distance to the nucleus, wider than fully developed bow shocks.<ref>{{cite journal |title=The infant bow shock: a new frontier at a weak activity comet |journal=[[Astronomy & Astrophysics]] |last1=Gunell |first1=H. |last2=Goetz |first2=C. |last3=Simon Wedlund |first3=C. |last4=Lindkvist |first4=J. |last5=Hamrin |first5=M. |last6=Nilsson |first6=H. |last7=LLera |first7=K. |last8=Eriksson |first8=A. |last9=Holmström |first9=M. |display-authors=1 |volume=619 |at=L2 |date=November 2018 |doi=10.1051/0004-6361/201834225 |bibcode=2018A&A...619L...2G |url=https://www.duo.uio.no/bitstream/10852/67125/1/aa34225-18.pdf |archive-url=https://web.archive.org/web/20190430061032/https://www.duo.uio.no/bitstream/10852/67125/1/aa34225-18.pdf |archive-date=2019-04-30 |url-status=live|doi-access=free }}</ref>