00ASUN.README
*** see end below for irradiance ***
SPECTRUM COMPUTED FOR ATLAS9 MODEL ASUN. LTE, PLANEPARALLEL, 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)**(I1),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 8.808E04 1.082E03
300009.49066388 7.140E04 1.082E03
300010.09068286 5.055E04 1.082E03
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=200300000NM

 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 = 2.720E4 .
To convert from erg/cm**2/s/nm to W/m**2/micron
multiply by 1.E7*1.E4*1.E3 = 1.