Model Spectral Energy Distributions
Below are the data files for SEDs for a PASSIVE disk presented in our
2002 paper ``Infrared Signatures of Protoplanetary Disk Evolution.''
The star and disk parameters are: T*=4000K, R*=2Rsun, Rdisk=100AU,
Rin=8R*, h0=0.017R*, beta=1.25, alpha=2.25. The parameters
describing the disk density structure are set out in the paper.
The dust opacity is described in our HH 30 IRS modeling paper.
The disk mass is varied from 1.e-8 to 0.1Msun. There are 10 SEDs in each
model data set, evenly spaced in cos(inclination).
The columns
are wavelength (microns), total flux, direct stellar flux, scattered flux,
and thermal flux (all in normalized lambda*F_lambda). To convert to real
units (ergs/s/cm^2), multiply by sigma*Tstar^4*(Rstar/d)^2,
where d is the source distance and sigma is the Stefan-Boltzmann constant.
An IDL program to read in the model and
display it alongside the input stellar spectrum is provided. The IDL
program is set up to display the models assuming a source distance of 140pc.
The SEDs below are for the set of parameters described above
and the disk mass is varied. We intend to make a library of disk
models varying all parameters. If you want SEDs for particular disk
and star parameters, just send me an email and I'll run them for you.
The low resolution models below only took a few minutes each to produce.
Longer runs, giving higher signal to noise SEDs, can be run on request.
The models below are for PASSIVE disks only. We are currently
working on a paper presenting SEDs for Class I envelope + disk sources
(Whitney et al. 2002). At some stage all the SED models and codes will
be made available. Until then, feel free to ask if you want us to run
any particular geometry/illumination model.
IDL program:
sed.pro
Input 4000K Kurucz model atmosphere:
flx4000kg35.dat
Dust opacity file. Columns are wavelength (microns), total opacity
(cm^2/g), albedo, Heyney-Greenstein asymmetry parameter:
dust.dat
Model SED data files:
M_d = 1.e-2 Msun: f_m-2.dat
M_d = 1.e-3 Msun: f_m-3.dat
M_d = 1.e-4 Msun: f_m-4.dat
M_d = 1.e-5 Msun: f_m-5.dat
M_d = 1.e-6 Msun: f_m-6.dat
M_d = 1.e-7 Msun: f_m-7.dat
M_d = 1.e-8 Msun: f_m-8.dat
Updated: April 2002