00ASUN.README
*** see end below for irradiance ***
SPECTRUM COMPUTED FOR ATLAS9 MODEL ASUN.  LTE, PLANE-PARALLEL, NO CHROMOSPHERE
TITLE TEST RUN SOLAR MODEL WITH SDSC OPACITY  VTURB 1.5 KM/S    L/H 1.25
TEFF  5777.
GRAV  4.4377
ABUND [0.0]              Anders and Grevesse 1988
VTURB 1.5 km/s
HE 0.089
VROTATION  2.0 km/s
VMACRO 1.5 km/s
Wavelength, flux, continuum triplets
  in vacuum nm and in ergs/cm**2/s/ster/nm
(WL(I)=FIRSTWL*(1.D0+1.D0/RESOLUTION)**(I-1),I=1,NWL)
FIRSTWL     150.00025431
LASTWL   300010.09068286
RESOLUTION        500000  (actually resolving power)
NWL              3800472
     150.00025431 4.514E+00 5.608E+00
     150.00055431 4.645E+00 5.608E+00
     150.00085431 4.769E+00 5.609E+00
 
  300008.89064610 8.808E-04 1.082E-03
  300009.49066388 7.140E-04 1.082E-03
  300010.09068286 5.055E-04 1.082E-03
 
The spectrum was computed with the same lines that were used to compute
the ATLAS12 model.  Lines with good wavelengths should match features in
an observed spectrum.  The predicted lines can have a large wavelength
uncertainty.
 
The 500000 resolving power spectrum was instrumentally broadened with a
gaussian to smaller resolving powers at the same wavelengths using program
BROADEN. The broadened spectra were then resampled at the center of an odd
number of points using program RESAMPLE.  The new points are uniformly
spaced in doppler space.
 
     wl interval nm end  ALL=200-300000NM
     |
     |   resolving power
     |    |       resampling divisor
     |    |       |             blocks =512B
FSUNALLP.100                       282067
FSUNALLP.1000                      282067
FSUNALLP.10000                     282067
FSUNALLP.100000                    282067
FSUNALLP.100000RESAM3               94023
FSUNALLP.10000RESAM25               11283
FSUNALLP.1000RESAM251                1124
FSUNALLP.100RESAM2501                 113
FSUNALLP.200                       282067
FSUNALLP.2000                      282067
FSUNALLP.20000                     282067
FSUNALLP.20000RESAM13               21698
FSUNALLP.2000RESAM125                2257
FSUNALLP.200RESAM1251                 226
FSUNALLP.300                       282067
FSUNALLP.3000                      282067
FSUNALLP.30000                     282067
FSUNALLP.30000RESAM9                31341
FSUNALLP.3000RESAM83                 3399
FSUNALLP.300RESAM833                 8548
FSUNALLP.500                       282067
FSUNALLP.5000                      282067
FSUNALLP.50000                     282067
FSUNALLP.500000                    282067
FSUNALLP.50000RESAM5                56414
FSUNALLP.5000RESAM51                 5531
FSUNALLP.500RESAM501                  563

                       Irradiance

     The fluxes I compute from my model atmosphres are flux 
moments at the surface of the star in ergs/cm**2/s/ster/nm.
The solar irradiance is the flux at 1 AU from the center of 
the sun.  

     To convert from flux moment to irradiance multiply by   
4*pi*(Rsun/AU)**2 = 2.720E-4 .   

     To convert from erg/cm**2/s/nm to W/m**2/micron 
multiply by 1.E-7*1.E4*1.E3 = 1.