8 A. CASTRO AND V. PADR
´
ON


d
D
1
λ
μ1
p−q
ν2
p−q
μ2
p−q
ν3
p−q
μ3
p−q
νn
p−q
μn
p−q
ψ2 ψ3 ψn
ξ1 ξ2 ξ3 ξn
Figure 1. Bifurcation curves defined by the functions ξj (contin-
uous line), and ψj (dotted line) for the case 1 q p
N+2
N−2
.
the absence of a magnetic field and constant heating per unit of mass or constant
heating per unit of volume.
In Figure 6 the number of absorbing zones is bounded in terms of the radius of
the star. For very large radii there are steady states with large number of absorbing
zones. This case includes n 3/2 for plasma diffusing perpendicular to a magnetic
field and constant heating per unit of mass or constant heating per unit of volume.
When q −1, and 1 p
N+2
N−2
Figure 7 shows that for any radius there
are infinitely many possible steady state configurations. However, the number of
absorbing zones decays with the radii. Also for very low temperatures the radius
must approach special values in terms of the number of absorbing zones.
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