Library of Stationary PDR Models

                              B.T. Draine
                    Princeton University Observatory
                Peyton Hall, Princeton NJ 08544-1001, USA
                         draine@astro.princeton.edu

                                   and 

                            Frank Bertoldi
             Max-Planck-Institut fur Extraterrestrische Physik
                       D-85748 Garching, Germany
                        fkb@mpe-garching.mpg.de

                        (last modified 97.09.30)

The ftp directory draine/pdr contains H2 quadrupole emission spectra 
calculated for 24 models of stationary photodissociation fronts.  The physical 
assumptions and method of calculation is described by Draine & Bertoldi (1996),
and some of the results for these models (e.g., 1-0S(1) surface brightnesses)
are presented there.

Please note one ***IMPORTANT CHANGE***: due to a numerical error in the 
original pdr code, the model results presented by Draine & Bertoldi (1996) 
were actually computed using an H2 formation rate given by

   dn[H_2]                  
   ------- = 3 * 10^{-18} * sqrt(T/K) * n(H) * n_H cm^3 s-1                (1)
     dt

instead of the coefficient of 6*10^{-18} stated in the text.  [This error was
discovered recently, and an erratum is being submitted to Ap.J.]  The
results presented in this directory assume the formation rate of eq. (1), 
and therefore are consistent with the model results presented in Draine &
Bertoldi (1996).

In addition, we note that the model results which were stored in this
directory prior to 97.09.30 inadvertently failed to list O(2) lines (due to
an oversight in the program used to prepare the line lists).  O(2) lines
are included in the spectra tabulated here.

Intensities are given for all of the H2 quadrupole lines with intensities
exceeding 0.1% of the intensity of the 1-0S(1) line.  Intensities are 
calculated for viewing angle theta (theta=0 is "face-on").

For each model, the spectrum is contained in a file 'spdf.irs.modl'
where 'modl' is a string identifying the model.  26 models are available:


	Model	n_H	chi   sigma_d	 T_0  cos(theta)
	       (cm-3)        (1e-22cm2)  (K)
	-----------------------------------------------
	am3d	10^2	 1	20	 300	1
	am3o	10^2	 1	 6	 300	1
	aw3d	10^2	 1	20	 500	1
	aw3o	10^2	 1	 6	 500	1
	bw3d	10^2	10	20	 500	1
	bw3o	10^2	10	 6	 500	1
	bh3d	10^2	10	20	1000	1
	bh3o	10^2	10	 6	1000	1
	Bm3o	10^3	10	 6	 300	1
	Bw3o	10^3	10	 6	 500	1
	Cw3o	10^3	10^2	 6	 500	1
	Ch3o	10^3	10^2	 6	1000	1
	Gm3o	10^4	10^2	 6	 300	1
	Gw3o	10^4	10^2	 6	 500	1
	Hw3o	10^4	10^3	 6	 500	1
	Hh3o	10^4	10^3	 6	1000	1
	Iv3o	10^4	10^4	 6	1500	1
	Ix3o	10^4	10^4	 6	2000	1
	Jv3o	10^4	10^5	 6	1500	1
	Jx3o	10^4	10^5	 6	2000	1
	Lm3o	10^5	10^3	 6	 300	1
	Lw3o	10^5	10^3	 6	 500	1
	Mw3o	10^5	10^4	 6	 500	1
	Mh3o	10^5	10^4	 6	1000	1
	Mv3o	10^5	10^4	 6	1500	1
	Mx3o	10^5	10^4	 6	2000	1
	Nv3o	10^5	10^5	 6	1500	1
	Nx3o	10^5	10^5	 6	2000	1
	Ov3o	10^5	10^6	 6	1500	1
	Ox3o	10^5	10^6	 6	2000	1
	Qm3o	10^6	10^4	 6	 300	1
	Qw3o	10^6	10^4	 6	 500	1
	Qv3o	10^6	10^4	 6	1500	1
	Qx3o	10^6	10^4	 6	2000	1
	Rw3o	10^6	10^5	 6	 500	1
	Rh3o	10^6	10^5	 6	1000	1
	Rv3o	10^6	10^5	 6	1500	1
	Rx3o	10^6	10^5	 6	2000	1
	Sv3o	10^6	10^6	 6	1500	1
	Sx3o	10^6	10^6	 6	2000	1
	n2023a	10^5	5000	 6	 500	0.2
	n2023b	10^5	5000	 6	 900	0.2

n_H	= H nucleon density (assumed constant throughout the PDR)

chi	= uv intensity incident on PDR, in units of Habing intensity
	  (see eq. ?? of Draine & Bertoldi 1996).

sigma_d	= effective dust attenuation cross section at 1000A
	  sigma_d=20e-22 cm2 for "diffuse cloud dust" with R_V=3.1;
	  sigma_d= 6e-22 cm2 for "dense cloud dust" with R_V=5.5

T_0	= parameter determining temperature profile of PDR (see eq.41
	  of Draine & Bertoldi (1996): T = T_0/(1+tau_{d,1000})

theta	= viewing angle (theta=0 is "face-on").

If you are interested in H2 vibration-rotation spectra for PDRs characterized
by other values of n_H, chi, sigma_d, T_0, or cos(theta), contact
draine@astro.princeton.edu .

References:

Draine, B.T., \& Bertoldi, F. 1996, "Structure of Stationary Phodissociation
Fronts", Ap. J., 468, 269