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A Method of Computing General Perturbations of
Intensity of Forbidden Lines and Abundance
Results of Recent Precise Levelling along
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absorption abundance ratio Aller Balmer continuum limit Balmer decrement Balmer line Boltzmann equation Bull central star coefficients column of Table computed condition for radiative denotes determined deviation Earthq effect electron velocity distribution electron-temperature emission expansion fluxes forbidden lines free electrons free-free frequency function gaseous assembly given in Table Hagihara Hence Hermite polynomials incident radiation intensity ratio ionisation ions Latitude Lyman continuum Lyman series Lyman series lines Maxwellian electron velocity Maxwellian velocity distribution Menzel model planetary nebulae nebula in radiative nebular lines non-Maxwellian nuclear temperature number of free numbers of atoms numerical values observations obtained optical depth optical thickness orbital outer boundary planetary nebulae potential gradient present paper Proper Motion pure capture radiative equilibrium radiative transfer Randverdunkelung result Right Ascension second approximation shown slow electrons spectral intensity spectral intensity distribution steady superelastic thunderstorm tion Tokyo Astr Tokyo Imperial University unit volume values of 32 various quantum