Input for ATMOS

PTAU.DAT

Example (Holweger-Müller solar model):

 5780.00  4.44   -1.00  5000.00                            Teff  log g   -1   lambda ref
 29                                                        # of depth points
 2.891E-07 5.260E-07 1.355E-06 2.582E-06 4.634E-06         
 9.977E-06 1.791E-05 3.266E-05 7.396E-05 1.393E-04         29 tau_5000 values
 2.649E-04 6.310E-04 1.225E-03 2.393E-03 5.848E-03
 1.151E-02 2.265E-02 5.546E-02 1.094E-01 2.685E-01
 4.256E-01 7.362E-01 1.045E+00 1.552E+00 2.051E+00
 3.954E+00 5.768E+00 7.534E+00 9.268E+00
 -1                                                        temperatures follow
  3900.  3920.  3970.  4030.  4080.                        29 temperatures [K]
  4160.  4210.  4270.  4340.  4400.
  4460.  4530.  4590.  4640.  4720.
  4800.  4900.  5080.  5260.  5560.
  5850.  6260.  6570.  6880.  7160.
  7920.  8250.  8420.  8500.
  1.35                                                     microturbulence [km/s]
   2   1   1   1   1   1   1
  30                                                       # of wavelengths
   2200.00   2300.00   2490.00   2495.00   2515.00
   2520.00   2880.00   2930.00   2950.00   2960.00         30 wavelenghts [Å]
   3445.00   3450.00   3460.00   3520.00   3590.00
   3630.00   3650.00   3700.00   4000.00   5000.00
   6000.00   7000.00   8050.00   8150.00   8210.00
   8215.00   9000.00  10000.00  12000.00  14000.00
 29                                                        # of depth points

Specifications and Details:

first line Teff logg RSU lambda ref
F8.2 F6.2 F8.2 F9.2
Effective Temperature Gravity
log g1
Radius in solar radii
For calculation of pressure stratification:
If RSU <= 0:
plane parallel stratification with
log g=const
(Parameter is not really used in this case)
RSU >0:
spherical approximation with
log g= log g1 + 2 log (R( tau1)/R(tau) )
where subscript 1 stands for the outermost layer.
reference wavelength [Å] for optical depth scale
2nd line I number of depth points (I3)
I=0
use 30 point standard optical depth scale
I>0
read monochromatic optical depth scale from next lines, 5 numbers per line (5E10.3)
(2+I)th line M control flag (I3)
M = 0 scaled solar HM model (built in): T(tau) = TSun(tau) ·Teff/5780
M = 1 theta (5040/T) values for each depth point follow, I many, 5 per line (5F7.4)
M = -1 T values for each depth point follow, I many, 5 per line (5F7.0)
(2+I+M)th line TUR microturbulence (F6.2)
TUR < 0 depth dependent microturbulence [km/s]; values follow for every depth point, I many, 5 per line (5F7.2)
TUR > 0 micro=TUR [km/s] for all depth points
next line MODE, IONST, IPRINT, KPRINT,   LPR1, LPR2, LPRD,   KPID, PLMIN, PLMAX, KPKT
7 to 9 control flags (free format)
a) MODE
=1: IONDIS computes particle concentrations ZETAJ only for the usually important elements
=2: IONDIS computes particle concentrations for all elements it knows about
(computation of pressure stratification (pgas and DENSNC) is always done with important elements only)
b) IONST
ignored (not used anymore)
c) IPRINT
=1: no output from IONDIS
=2: IONDIS prints ionization equilibria and similar for depth points specified below
d) KPRINT
=1: no output from OPALAM
=2: OPALAM prints details for opacities for all wavelengths
=4: make a file suitable for plotting with program OPAPLOT
e-g) LPR1,LPR2,LPRD
first depth point, last depth point, and increment for printing of details
h-k) KPID,PLMIN,PLMAX,KPKT (optional if KPRINT!=4)
KPID: # of depth point for plot
PLMIN,PLMAX: wavelength interval
KPKT: # of wavelength points for plot
(3+I+M)th line NLAKS # of wavelengths for computation of continuous opacities (free format)
NLAKS=0: use the following 12 standard wavelengths (good for optical and IR only):
  3648,  4000,  5000,  6000,  7000,
  8000, 10000, 12500, 15000, 16420,
 20000, 25000 [Å]
NLAKS>0: list the desired NLAKS wavelengths on the following lines, 5 per line (5F10.2)
last line LCONTR# of depth points again for consistency check. Must be 30 if I=0. (I3)