Resumo (PT):
The aim of this work is to find the condition for the existence of convective cores in homogenous main sequence stars where the opacity per unit mass is k=k_0ρ^α T^-β and the energy generation rate per unit mass is ɛ=ɛ_0ρT^η (ρ and T being the density and the temperature, respectively).
Numerical models of stars with different values of α, β and η are constructed and the condition for the existence of a convective core in terms of the relation between α, β and η determined.
Forty points η=η(α,β) are determined for αin[0,2] and βin[0,4] and the condition is found to be η = - 3.3294 α + 2.0243 β + 1.8393
Abstract (EN):
The aim of this work is to find the condition for the existence of convective cores in homogenous main sequence stars where the opacity per unit mass is k=k_0ρ^α T^-β and the energy generation rate per unit mass is ɛ=ɛ_0ρT^η (ρ and T being the density and the temperature, respectively).
Numerical models of stars with different values of α, β and η are constructed and the condition for the existence of a convective core in terms of the relation between α, β and η determined.
Forty points η=η(α,β) are determined for αin[0,2] and βin[0,4] and the condition is found to be η = - 3.3294 α + 2.0243 β + 1.8393
Language:
Portuguese
Type (Professor's evaluation):
Scientific
Notes:
Orientador: Ian W. Roxburgh
No. of pages:
50