... Formation0.1
http://yso.mtk.nao.ac.jp/~tomisaka/Lecture_Notes/StarFormation/5.pdf 
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... stars1.1
However, the same authors (Ikeda and Kitamura 2009) obtained $n\simeq -2.3\pm 0.3$ even for C$^{18}$O cores (its critical density $\sim 10^3{\rm cm}^{-3}$) in OMC-1 region in the Orion A cloud. 
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... them4.1
One of the reasons why large increase in the mass/flux ratio is favored is understood as follows: There have been a long-standing ``magnetic flux problem of stars'' in which the magnetic flux of, say, $1M_\odot$ main-sequence star $\Phi\sim XX{\rm G cm^2}$ is much smaller than that of the parent cloud $\Phi\sim XX{\rm G cm^2}$. The magnetic flux must be reduced in the star formation process. If the mass-flux ratio increases much in these density range, this might resolve the magnetic flux problem of stars. 
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...) 4.2
This means $A=2+\epsilon$ and $\epsilon>0$ and $\rightarrow 0$ 
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... stateC.1
Reference book for this appendix is chapter 4 of Chandrasekhar (1939). 
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