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((refimprove|date=March 2017))
A '''champagne flow''' is an [[astrophysical]] event whereby an [[HII region]] inside a molecular cloud expands outward until it reaches the interstellar medium. At that point, the ionized [[hydrogen]] [[gas]] bursts outward like an uncorked champagne bottle. This event is also sometimes called a Blister.<ref>((cite book|last1=Franco|first1=Jose|last2=Ferrini|first2=Federico|last3=(Ed)|first3=G. TENORIO-TAGLE|title=Star Formation, Galaxies and the Interstellar Medium|date=10 June 1993|publisher=[[Cambridge University Press]]|isbn=9780521444125|page=241|url=https://books.google.com/books?id=4g9sT_xZp3gC&pg=PA241|language=en))</ref> An HII region is created by [[ionization]] from a recently formed star (usually an [[OB star|O-star]]) inside a molecular cloud.

The champagne model is perhaps one of the first [[numerical calculation]]s of the propagation of [[ionisation]] fronts and of the expansion of [[HII region]]s that 
did not assume a constant density medium around the massive exciting [[star]]. The model assumes that 
[[star formation]] takes place in a dense cloud, surrounded and in pressure equilibrium with a low density inter-cloud gas.
The ample supply of [[UV photon]]s generated by the star rapidly establishes an HII region and the expansion of this, sooner or later 
allows also for the ionisation of the inter cloud gas. Ionisation disrupts then the former pressure balance between the 
cloud and the inter-cloud gas as under the stellar radiation field all photo-ionised gas acquires a temperature of the order of 10000 K.
In this way, the ionised cloud material acquires an excess pressure, a pressure larger than the ionised low density inter cloud gas and this 
provoques the supersonic expansion of the ionised cloud matter into the surrounding gas (the champagne flow). The streaming of matter out of the cloud allows 
for the ionisation of a larger portion of the original cloud sustaining in this way the pressure imbalance which eventually leads to the complete disruption
of the parent cloud.   The terms champagne model and champagne flow were coined by [[Mexico|Mexican]] astrophysicist Guillermo Tenorio-Tagle in a paper in 1979 (Astronomy and Astrophysics 1979A&A....71...59T).
The model focus on the  size, [[velocity field]] and the large density variations observed in HII regions.  This article was followed by further [[hydrodynamical]] 
calculations  in one and two dimensions, in collaboration with Drs. Peter Bodenheimer, Harold W. Yorke and Piet Bedijn see:1979ApJ...233…85B.1983A&A...127..313Y,  1979A&A....80..110T,  1982ASSL...93….1T,  1984A&A...138..325Y,  1981A&A....98…85B

==References==
((reflist))

==Further reading==

* ((cite journal |last1=Garay |first1=Guido |last2=Lizano |first2=Susana |title=Massive Stars: Their Environment and Formation |journal=Publications of the Astronomical Society of the Pacific |volume=111|issue=763 |year=1999 |pages=1049–1087 |doi=10.1086/316416|arxiv = astro-ph/9907293 |bibcode = 1999PASP..111.1049G |s2cid=119495055 ))
* ((cite journal |last=Tenorio-Tagle |first=G. |title=The Gas Dynamics of HII Regions. I. The Champagne Model |journal=Astronomy and Astrophysics |year=1979 |volume=71 |pages=59–65 |bibcode=1979A&A....71...59T))

((DEFAULTSORT:Champagne Flow))
[[Category:Astrophysics]]


((Astrophysics-stub))

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