version 1.1, 2019/02/22 22:26:44

version 1.2, 2019/02/24 18:34:11

Line 97 background mass density is constant over 

Line 97 background mass density is constant over 

for plots of single modes, we do not scale the displacement amplitudes  for plots of single modes, we do not scale the displacement amplitudes 
by frequency to get a velocity, because this would also be invisible.  by frequency to get a velocity, because this would also be invisible. 
when we begin adding modes together, however, we must properly account  when we begin adding modes together, however, we must properly account 
for their relative amplitudes. so in this case the frequency scaling is 
for their relative amplitudes, so in this case the frequency scaling is 
necessary because the frequency will be different for different modes.  necessary because the frequency will be different for different modes. 
 
 
Line 268 and radial order n. finally, we will al 

Line 268 and radial order n. finally, we will al 

density used to construct the model.  density used to construct the model. 
 
all of this data has been packaged into an hdf file available from the  all of this data has been packaged into an hdf file available from the 
SoSH website: http://solarcenter.stanford.edu/SoSH/#mods 
SoSH website: http://solarcenter.stanford.edu/SoSH/#mods . at the 

beginning of each of these scripts, we call the function loadmodel(), 

which reads the mesh and mass density used for the model, as well as the 

l, n and frequency of all the modes in the model, and puts them in 

global variables. a second function, getradial(l, n), will return the 

actual displacement eigenfunctions for the modes we wish to plot. 



after loadmodel(), the scripts call image2rtheta(), which returns the 

arrays containing the r and theta coordinates for each point in the 

image. like its surface counterpart, this function can take as 

arguments the number of pixels in the x and y directions (default 1000). 

the only other paramter it can take, however, is distobs, the observer 

distance in solar radii. in other words, the orientation of the rtheta 

plane is fixed. distobs should in general be set to the same value used 

for the surface views; in both cases it defaults to 220. note, however, 

that these scripts can take another parameter, rsurf, which is the 

fractional image radius at which to truncate the model (default 1.0). 

in some cases you may wish to remove the surface values if you find they 

dominate the plots. this will reduce the size of the area occupied by 

the plot. 



as mentioned above, the radial eigenfunctions will be scaled by the mass 

density. for the value of phi in drawradial.py, we have arbitrarily 

chosen pi/4m for the right half of the image, so that the real and 

imaginary parts of the spherical harmonic (recall the factor of 

exp(imphi)) will be the same. this means that all three components will 

be comparable. of course, the value of phi on the left half of the 

image will be pi/4m + pi. for m=0, we set phi=0. in addradial.py, we 

set phi according to the first mode entered. 
 