real teff f=F13.3 b=4 n='Effective Temperature' u=K 3500.0(for a relatively cool star). Note that the actual effective temperature can only be determined a posteriori and that the entropy of the instreaming entropy (see below) is more important than
teffitself. In fact,
teffis only used to control material properties at the outer boundary. Its value should be close to the expected effective temperature of the model.
character grav_mode f=A80 b=80 n='Type of gravity field' & c0='constant/central' centralTwo values are possible so far:
constant: In the standard ``solar'' case the constant gravity specified with
real gravis directed downward in x3 direction.
central: For the ``supergiant'' case a central potential is assumed with an origin at x=0. The stellar mass as well as inner and outer smoothing radius have to be specified.
real grav f=E15.8 b=4 n='Gravity' u=cm/s^2 27500.0Setting this value to zero switches off gravity (oh wonder).
real mass_star f=E15.8 b=4 n='Stellar Mass' u=g 9.94500e+33
r0_grav, specified with
real r0_grav f=E15.8 b=4 n='Inner Smoothing Radius' u=cm 9.45833e+12This parameter should always be non-zero for a central potential.
r1_grav, specified with
real r1_grav f=E15.8 b=4 n='Outer Smoothing Radius' u=cm & c0='0.0: Not used' 11.35000e+13Setting this parameter to zero gives the usual 1/r behavior of the potential in the outer layers but also chooses another smoothing formula in the central part (where
real r0_gravis relevant). But a value somewhat larger than the remotest corner of the box effectively cancels this artificial smoothing in the outer layers without changing the formula for the potential.