1201.0483 (L. B. Lucy)
L. B. Lucy
A two-component phenomenological model developed originally for zeta Puppis
is revised in order to model the outflows of late-type O dwarfs that exhibit
the weak-wind phenomenon. With the theory's standard parameters for a generic
weak-wind star, the ambient gas is heated to coronal temperatures ~ 3 x 10^{6}K
at radii > 1.4 R, with cool radiativly-driven gas being then confined to dense
clumps with filling factor ~ 0.02. Radiative driving ceases at radius ~ 2.1R
when the clumps are finally destroyed by heat conduction from the coronal gas.
Thereafter, the outflow is a pure coronal wind, which cools and decelerates
reaching infinity with terminal velocity ~ 980$ km/ s.
View original:
http://arxiv.org/abs/1201.0483
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