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Illustration by Francis Barlow, 1687.

ÆSOPUS 1.0 input form

Low-temperature Rosseland mean opacities
on demand

See the paper Marigo & Aringer (2009) for code details,
and Marigo et al. (2022) for the latest updates.
A new AESOPUS 2.0 interface is here.

Help

After submission, please wait for the output file to appear

Temperature and density grid Specify the limits and the variation step of the state variables:

log T from to
in steps of dex up to , then changing to dex.

log R from to in steps of dex

Chemical composition First choose the reference solar composition, the reference metallicity Zref, and the grid of hydrogen abundance X:

Reference solar composition
Anders & Grevesse (1989; AG89)
Grevesse & Noels (1993; GN93)
Grevesse & Sauval (1998; GS98)
Holweger (2001; H01)
Lodders (2003; L03)
Grevesse, Asplund & Sauval (2007; GAS07)
Asplund et al. (2009; AGSS09)
Caffau et al. (2011; C11)
Asplund et al. (2021; AAG21)
Magg et al. (2022; MBS22)

Reference metallicity Zref =

Hydrogen abundance X from to in steps of

Abundances normalization

Choose the normalization of the metal abundances, expressed as either number fractions or mass fractions
εi: Abundances in number fractions Xi: Abundances in mass fractions

Primordial mixture

In the case of a metal-free mixture, i.e. Zref=0, one can choose a primordial lithium abundance in terms of the ratio Li/H, using either number fractions, εLi/εH, or mass fractions, XLi/XH (depending on the abundances normalization selected in the previous step):

Lithium abundance Li/H=

Reference mixture with Z=Zref

Then define the kind of reference mixture (keeping Z constant):
scaled-solar mixture A mixture B

Ratios [Xi/XFe] =[εi/εFe], in dex, keeping the metallicity constant, Z=Zref
Li Be B C N O F Ne Na
Mg Al Si P S Cl Ar K Ca
Sc Ti Ga Ge As Se Br Kr Rb
Sr Y Zr Nb Mo Ru Rh Pd Ag
Cd In Sn Sb Te I Xe Cs Ba
La Ce Pr Nd Sm Eu Gd Tb Dy
Ho Er Tm Yb Lu Hf Ta W Re
Os Ir Pt Au Hg Tl Pb Bi Th
U

Superimposed chemical pattern with Z ≠ Zref

Then define the additional enhancement/depletion factor for any element, in dex:

Abundance variation factor of each element (in dex) relative to the reference mixture: gi=log10(εi)-log10(εi)ref or fi=log10(Xi)-log10(Xi)ref.
The metallicity is not preserved.
Li Be B C N O F Ne Na
Mg Al Si P S Cl Ar K Ca
Sc Ti V Cr Mn Fe Co Ni Cu
Zn Ga Ge As Se Br Kr Rb Sr
Y Zr Nb Mo Ru Rh Pd Ag Cd
In Sn Sb Te I Xe Cs Ba La
Ce Pr Nd Sm Eu Gd Tb Dy Ho
Er Tm Yb Lu Hf Ta W Re Os
Ir Pt Au Hg Tl Pb Bi Th U

(C/O) - C - N variation grid

OPTIONAL: define the grid of abundance variation factors (in dex) of C/O, C, N relative to the reference values:

gCO=log10(εC/εO)-log10(εC/εO)ref
gC=log10(εC)-log10(εC)ref
gN=log10(εN)-log10(εN)ref		 OR fCO=log10(XC/XO)-log10(XC/XO)ref
fC=log10(XC)-log10(XC)ref
fN=log10(XN)-log10(XN)ref

gCO or fCO values
gC or fC values
gN or fN values
This service is mantained by Paola Marigo and hosted at the Osservatorio Astronomico di Padova.
Questions, comments and special requests should be directed to paola.marigoatunipd.it .
Last modified: Fri Oct 14 11:00:59 2022