Editing Protostar (section)

==History==
The modern picture of protostars, summarized above, was first suggested by [[Chushiro Hayashi]] in 1966.<ref>{{Cite journal |title=The Evolution of Protostars |last=Hayashi |first=Chushiro |date=1966 |journal=Annual Review of Astronomy and Astrophysics |volume=4 |pages=171–192 |doi=10.1146/annurev.aa.04.090166.001131 |bibcode=1966ARA&A...4..171H }}</ref> In the first models, the size of protostars was greatly overestimated. Subsequent numerical calculations<ref>{{Cite journal|title = Numerical Calculations of the Dynamics of a Collapsing Protostar|last = Larson, R. B.|date = 1969|journal = Monthly Notices of the Royal Astronomical Society |volume=145 |issue = 3|pages=271–295|doi = 10.1093/mnras/145.3.271|bibcode = 1969MNRAS.145..271L |doi-access = free}}</ref><ref>{{Cite journal|title = Formation of Solar-Type Stars in Spherical Symmetry: I. The Key Role of the Accretion Shock|author1=Winkler, K.-H. A. |author2=Newman, M. J. |name-list-style=amp |date = 1980|journal = Astrophysical Journal |volume=236 |pages=201|doi = 10.1086/157734|bibcode = 1980ApJ...236..201W |doi-access=free }}</ref><ref>{{Cite journal|title = The Evolution of Protostars: I. Global Formulation and Results|last = Stahler, S. W., Shu, F. H., and Taam, R. E.|date = 1980|journal = Astrophysical Journal |volume=241 |pages=637|doi = 10.1086/158377|bibcode = 1980ApJ...241..637S }}</ref> clarified the issue, and showed that protostars are only modestly larger than main-sequence stars of the same mass. This basic theoretical result has been confirmed by observations, which find that the largest pre-main-sequence stars are also of modest size.