Table A.1: Opacity models cited in the text.

Model		 Composition Absorbers Quantities Validity Usage Studies
  Z dust gas $\kappa_{\rm R}$ $\kappa_{\rm P}$ T, K $\rho$, g  cm-3    

Cox &		 $10^{-4} \div 1$ - a* + - $1~500 \div 10^9$ $10^{-15} \div 10^{10}$ Wood Pulsations of
Stewart               (1976) luminous
(1970a,b)$^{\rm a}$                 helium stars

Alexander		 $10^{-3} \div 0.02$ + m** + - $700 \div 10^4$ $10^{-19} \div 10^{-2}$ Bodenheimer Protostellar
(1975)$^{\rm a}$               et al. (1990) collapse

Alexander		 $10^{-4} \div 2\times10^{-2}$ + m + - $650 \div 10^4$ $10^{-18} \div 10^{-2}$ Ruden & Protostellar
et al. (1983)$^{\rm a}$               Pollack (1991) collapse

Pollack et al.		 Solar + - +$^{\rm c}$ - $10 \div 2~500$ $10^{-14} \div 1$ Boss (1988), Molecular cloud
(1985)                 fragmentation;
                Lunine et al. brown dwarf
                (1989), atmospheres;
                Bodenheimer  
                et al. (1990), protostellar
                Ruden & collapse
                Pollack (1991)  

Sharp		 Solar, - m + + $2~10^3 \div 10^4$ $10^{-10} \div 10^{-3}$ Sackmann Evolution
(1992) 3 times             et al. (1993), of the Sun;
  enhanced             Finocchi & chemistry of
  CNO             Gail (1997) accretion discs

Alexander		 $0 \div 1$ + m + + $700 \div 10^4$ $10^{-16} \div 10^{-5}$ Huré (2000), Accretion
& Ferguson                 discs of AGN
(1994) $^{{\rm a; b}}$                 and YSO;
                Driebe et al. evolution
                (1999), of helium
                  dwarfs;
                Ikoma et al. formation
                (2001) of giant
                  planets

Bell & Lin		 Solar + a +$^{\rm d}$ - $10 \div 10^6$ $10^{-20} \div 10^{-4}$ Bell & Lin FU Orionis
(1994)               (1994) outbursts

Pollack et al.		 Solar + - +$^{\rm c}$ - $10 \div 2\times10^3$ $10^{-18} \div 10^{-4}$ Huré (2000) Accretion
(1994)                 discs

Seaton et al.		 $0 \div 1$ - a + + $3\times10^3 \div 10^7$ $10^{-15} \div 10^{-2}$ Aikawa & Nonlinear
(1994) $^{{\rm a; b}}$               Antonello pulsations
(OP project)               (2000aa,b), of Cepheids,
                Aikawa (2001), accretion
                Huré (2000) discs

Henning &		 Solar + - + $^{{\rm c; d}}$ - $10 \div 2\times10^3$ $10^{-18} \div 10^{-4}$ Bell et al. Accretion
Stognienko               (1997) discs
(1996)$^{\rm b}$                  

Iglesias &		 $0 \div 2~10^{-2}$ - a + - $5\times10^3 \div 5\times10^8$ $10^{-15} \div 10^5$ Turcotte et al. Solar
Rogers               (1998), evolution,
(1996) $^{{\rm a; b}}$                  
(OPAL               Collins et al. accretion
project)               (1998) discs

Helling et al.		 Solar, - m +$^{\rm c}$ +$^{\rm c}$ $500 \div 10^4$ $10^{-19} \div 10^{-9}$ Helling et al. Dusty shells of
(2000) $^{\rm b}$ LMC,             (2000) long-period
  SMC$^{\rm e}$               variables
*
Atomic opacities.
**
Molecular and atomic opacities.
$^{\rm a}$
A trapezoidal table in $\rho$-T parameter space.
$^{\rm b}$
It can be retrieved via E-mail or the Internet.
$^{\rm c}$
Only plots are available.
$^{\rm d}$
Analytical expressions are used.
$^{\rm e}$
LMC, SMC mean the element abundances of the Large and the Small Magellanic Clouds.


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