Polarization and limb darkening of plane-parallel atmospheres
for 12 wavelengths between 3400A and 6000A.
These results were extracted from MARCS model atmospheres with
abundances 1/10 solar and 1 km/sec microturbulence.
Each file is from one atmosphere: Notation: P35g40 --> T_eff= 3,500K,
log g= 4.0, and also P425g45 --> T_eff= 4,250K, log g= 4.5.
There are 39 rows in each file, each with 159 numbers. The first
row is 159 values of $/mu$. The second row are the corresponding
values of $\theta = \acos(\mu)$ in radians, while the third row
are the values of $\theta$ in degrees. The polarization is highest
for \mu near zero (i.e., radiation emerging nearly parallel to the
surface of the stellar atmosphere), and varies rapidly as \mu goes
to zero, so I have spaced the values of \mu more closely there.
The next 3 rows (4,5,6) are values of I(\mu), Q(\mu) and the
polarization p(\mu)= Q(\mu)/I(\mu) for a wavelength of 6000A.
The following sets of three rows are I, Q and p for different
wavelengths. The 12 wavelengths are:
6000A 5500 5200 5000 4800 4600 4400 4200 4000 3800 3600 3400A
Note: The Planck function was normalized to unity at an optical depth
~2/3, so the absolute scale of the Stokes I & Q are arbitrary.