Stellar Continuum with Flux

I will try another approach to solve the flux calculation problem I am having in the codes. I will calculate each component of the profile separately, doing one step at a time. First only the continuum coming from the star, then see what happens with the continuum under the optical depths of the magnetosphere, and the wind, but without the flux contribution from these sources. In this way I can see if the absorptions on the continuum are in the right place, and the velocities are right. Then I will calculate only the magnetospheric contribution to the profile, and I will do the same to the diskwind component. Then I can see where the broad wings are coming from. After figuring that out, I will finally and both component to the stellar continuum, and I hope to have a good profile at last.

During my first continuum calculation I noticed a problem that was happening for velocities just higher than zero velocity. I forgot to bypass the optical depth test, and with that the code bypassed all the continuum calculations from those velocities. After ignoring the optical depth test in 'intens.f', I have the right continuum again. I guess this problem might be linked to the always present deep red shifted absorption (more than expected, and every time) found in all the profiles calculated so far. I need to take a deeper look at that.

The continuum calculated is in the file named 'prof.60.ha.mmax_7700K.dmax_7700K.continuum'. That is for a 60 degree inclination, the h-alpha line, maximum temperature in the magnetospheric funnel of 7700K, and maximum temperature in the diskwind region of 7700K. The stellar parameters are for a typical Classica T Tauri Star:

• Mass: 0.5 Msun
• Radius: 2.0 Rsun
• Photospheric Temperature: 4000K
• Accretion Ring Temperatura: 8000K
• Mass Accretion Rate: 1e-8 Msun/Year
• Mass Loss Rate: 1e-9 Msun/Year
• Magnetospheric Inner and Outer Radius: 3.0 Rstar and 3.3 Rstar
• Diskwind Inner and Outer Radius: 3.31 Rstar and 20.0 Rstar

The mass loss rate was calculated using the poloidal velocities in the base of the disk, and the densities in that region. The gas density that is used is a function of r and falls with r^(-1.5).

Obs: Just for you to remember. The intens.f have been changed to calculate only the continuum. I guess you will not forget that, but anyway...