An overview of the opacity models

The goal of this compilation is to provide an essential information about opacity models cited in the text. We show for which elemental composition they are developed, what kind of opacities they supply, and in what temperature and density ranges they work. In addition, the references to the studies where these opacity models have been applied are given and the aims of the investigations are briefly mentioned.

Primarily, we distinguish between two kinds of opacity models. The first kind is designed for stellar atmosphere modelling, where it is more convenient to use a special parameter, $R=\rho / T^3_6, {T}_6 = T / 10^6$ instead of gas density $\rho$ (see discussion in Rogers & Iglesias [1992]). Thus, opacity data of such models are assembled in rectangular tables in R-$T_6$ space. However, in hydrodynamical simulations of accretion discs, it is more convenient to have opacity tables composed in $\rho$-$T$ parameter space, for which we refer as to the second type of the models. The direct conversion of R to $\rho$ in the opacity models of the first kind leads to trapezoidal tables, where opacity values for different temperatures have different density intervals. We mark such models with ``a'' and show the maximum limits of density and temperature values for them.

In addition, we point out if opacity data are available on-line in the Internet or via E-mail (``b''). By default, the papers are supposed to contain the opacity data in a tabular form. Otherwise, when only opacity plots are available, we label the corresponding papers with ``c''.

Table: Opacity models cited in the text

Model	Composition,	Absorbers		Quantities		Validity		Usage	Studies
	Z	dust	gas	$\kappa_{\mathrm R}$	$\kappa_{\mathrm P}$	T, K	$\rho$, g cm$^{-3}$
Cox &	$10^{-4} \div 1$	-	+	+	-	$1\,500 \div 10^9$	$10^{-15} \div 10^{10}$	Wood	Pulsations of
Stewart								([1976])	luminous
([1970]a,b)$^{\mathrm a}$									helium stars
Alexander	$10^{-3} \div 0.02$	+	+	+	-	$700 \div 10^4$	$10^{-19} \div 10^{-2}$	Bodenheimer	Protostellar
([1975])$^{\mathrm a}$								et al. ([1990])	collapse
Alexander	$10^{-4} \div 2\,10^{-2}$	+	+	+	-	$650 \div 10^4$	$10^{-18} \div 10^{-2}$	Ruden &	Protostellar
et al. ([1983])$^{\mathrm a}$								Pollack ([1991])	collapse
Pollack et	Solar	+	-	+$^{\mathrm c}$	-	$10 \div 2\,500$	$10^{-14} \div 1$	Boss ([1988]),	Molecular cloud
al. ([1985])									fragmentation;
								Lunine et	brown dwarf
								al ([1989]),	atmospheres;
								Bodenheimer
								et al. ([1990]),	protostellar
								Ruden &	collapse
								Pollack ([1991])
Alexander	$0 \div 1$	+	+	+	+	$700 \div 10^4$	$10^{-16} \div 10^{-5}$	Huré ([2000])	Accretion
& Ferguson									discs of AGN
([1994]) $^{\mathrm{a; b}}$									and YSO
Bell & Lin	Solar	+	+	+$^{\mathrm d}$	-	$10 \div 10^6$	$10^{-20} \div 10^{-4}$	Bell & Lin	FU Orionis
([1994])								([1994])	outbursts
Pollack et	Solar	+	-	+$^{\mathrm c}$	-	$10 \div 2\,10^3$	$10^{-18} \div 10^{-4}$	Huré ([2000])	Accretion
al. ([1994])									discs
Seaton et	$0 \div 1$	-	+	+	+	$3\,10^3 \div 10^7$	$10^{-15} \div 10^{-2}$	Aikawa &	Nonlinear
al. ([1994]) $^{\mathrm{a; b}}$								Antonello	pulsations
(OP project)								([2000],[2000]),	of Cepheids,
								Aikawa ([2001]),	accretion
								Huré ([2000])	discs
Henning &	Solar	+	-	+ $^{\mathrm{c; d}}$	-	$10 \div 2\,10^3$	$10^{-18} \div 10^{-4}$	Bell et al.	Accretion
Stognienko								([1997])	discs
([1996])$^{\mathrm b}$
Iglesias &	$0 \div 2\,10^{-2}$	-	+	+	-	$5\,10^3 \div 5\,10^8$	$10^{-15} \div 10^5$	Turcotte et	Solar
Rogers								al. ([1998]),	evolution,
([1996]) $^{\mathrm{a; b}}$
(OPAL								Collins et	accretion
project)								al. ([1998])	discs
Helling et	Solar,	-	+	+$^{\mathrm c}$	+$^{\mathrm c}$	$500 \div 10^4$	$10^{-19} \div 10^{-9}$	Helling et	Dusty shells of
al. ([2000])$^{\mathrm{b}}$	LMC,							al. ([2000])	long-period
	SMC$^{\mathrm e}$								variables

$^{\mathrm a}$

a trapezoidal table in $\rho$-$T$ parameter space,

$^{\mathrm b}$

it can be retrieved via E-mail or the Internet,

$^{\mathrm c}$

only plots are available,

$^{\mathrm d}$

analytical expressions are used,

$^{\mathrm e}$

LMC, SMC mean the element abundances of the Large and the Small Magellanic Clouds,

$^{\mathrm f}$

monochromatic opacity plots are available only,