On 12/8/08, Valery Pipin <pip at iszf.irk.ru> wrote:
> real life example. Using the Peter's Eggleton stellar evolution code
> I've got a table of the stellar interior parameters for the Brown
> Dwarf (0.2 M_sun, 0.006 L_sun). The parameters are pressure,
> temperature, luminosity, density and etc.. . Now I want to use their
> functional form in my dynamo model. The best way is to get the
> Chebyshev approximations to them. I do as follows,
> 1) read the table to maxima
> 2) find the spline interpolation
> 3) find the Chebyshev approximations
Hey, that rocks. But I don't quite understand what's going on here.
Why is there both a cubic spline and a Chebyshev approximation?
I would have expected one or the other.
As always it is encouraging to see examples of real work with Maxima.
Robert Dodier