The complex recombination coefficient is adjusted adaptively to maximize the MMSE as measured on the recombination.
2.
The luminosity of the central star is denoted by L _ \ nu and \ alpha _ B is the recombination coefficient to the excited levels of hydrogen.
3.
Where is the " case B " recombination coefficient to the excited states of hydrogen, is the corresponding photoionization rate and " E " 21 = 10.2 eV is the energy of the first excited state.
4.
Where \ beta _ { n } ( T _ e ) is the recombination coefficient of the " n " th energy level in a unitary volume at a temperature T _ e, which is the temperature of the electrons in Kelvin and is usually the same as the sphere.
5.
Here F * is the " ionizing photon flux incident on the outside of the flow ", ? is the " initial velocity of the flow ", ? is the " recombination coefficient ", n 0 is the " peak ionized density in the flow ", and h, which is approximately 0.1 r 0, is the " effective thickness of the flow ".
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