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PONTIFICIAE ACADEMIAE SCIENTIARVM SCRIPTA VARIA

To complete the determination of the z-structure of the nebula, a further equation is needed, namely [Pg.56]

This completes the list of the needed equations. If one employs a theory (like the mixing length theory of convection) to compute Xc, as well as a model for the opacity kop, then eqs. (9) and (12) determine the vertical structure of the nebula, i.e. T, p and F vs. z, provided appropriate boundary conditions are imposed. These are usually taken to be [Pg.56]

the situation is more complex. For many years it was assumed that the major contribution to F came from Fr. However, it has been [Pg.56]

Equations (9) and (12) have been solved numerically by Lin and Papaloizou [Pg.57]

With the knowledge of these quantities, one can evaluate the mass of the nebula Mn, as well as the time scale for its evolution. The results are [Pg.58]

See other pages where PONTIFICIAE ACADEMIAE SCIENTIARVM SCRIPTA VARIA is mentioned: [Pg.8]    [Pg.10]    [Pg.12]    [Pg.14]    [Pg.16]    [Pg.18]    [Pg.20]    [Pg.28]    [Pg.34]    [Pg.36]    [Pg.38]    [Pg.42]    [Pg.46]    [Pg.48]    [Pg.50]    [Pg.52]    [Pg.54]    [Pg.56]    [Pg.58]    [Pg.60]    [Pg.64]    [Pg.66]    [Pg.72]    [Pg.74]    [Pg.76]    [Pg.78]    [Pg.80]    [Pg.84]    [Pg.90]    [Pg.92]    [Pg.94]    [Pg.96]    [Pg.100]    [Pg.102]    [Pg.104]    [Pg.106]    [Pg.108]    [Pg.112]    [Pg.116]    [Pg.118]    [Pg.122]    [Pg.124]    [Pg.128]    [Pg.130]    [Pg.136]    [Pg.140]    [Pg.142]    [Pg.144]    [Pg.146]    [Pg.148]    [Pg.150]   
See also in sourсe #XX -- [ Pg.56 ]



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