sme tutorial - stsci
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SME tutorial January 31 β February 2, 2011
Uppsala
Schedule
Monday
Short intro to SME
Installation and testing of the installation
Tuesday
3 exercises (creating SME input structure,
solving of global parameters, tuning line
parameters)
Starting to work on your data
SME physics
SME (= Spectroscopy Made Easy)
computes spectral synthesis and adjusts
free parameters based on comparison
with observations
SME spectral synthesis consists of
molecular and ionization equilibrium
solver EOS, continuous opacity package
CONTOP, line opacity package LINEOP
and RT solver RTINT
EOS
Abundances Zatom is the ratio natom / ntotal
is the number of particular
atoms in a particular species
(e.g. )
is the total number of atoms in a
particular species (e.g. )
charge of a given species:
Species
AtomX
2 2H O H O
H C2, 0X X
SpeciesX
2H O 3X
speciesqTiO+
H
1
1
q
q
Abundance and conservation
equations
Abundances (X is the number of atoms in a
given species):
Total number of particles:
Charge conservation (q is the electric charge):
Species
species Atom
species
Atom Species
species
species
n X
Zn X
species total
species
en n n P kT
species
species
species
en q n
Chemistry
Chemical reaction in which species A and B
form AB can be described by the chemical
equilibrium equation:
Ionization can be described in exact same way:
Saha equation!
3322
2
2( )
ABA B A B A B
AB AB AB
D
kTn n m m U UkTK T e
n h m U
32
2
22( )
Ae eA A
A A
I
kTn n Um kT
K T en h U
Using EOS
EOS has partition functions for 6 ionization stages of the first 99 atoms in the periodic table
EOS has partition functions for 257 molecules (up to four atoms) fitted over the range from 10K to 8000K
Input consists of T, P and abundances. Pe can be also imposed
EOS is using rather unique solving strategy making it robust
CONTOP
Continuous opacities are from ATLAS12
Modifications: partial pressures of
absorbers and their partition functions
are taken from EOS
List of absorbers: H, H2+, H-, He, He+, He-,
Si, Si+, Mg, Mg+, Al, C, Fe, Ca+, N, O, Ne, S,
List of scatterers: H, H2, He, e-
LINEOP
Given partial number densities of the line absorbers and their partition functions computes line opacities
Voigt profiles except for hydrogen lines
Natural, Stark and van der Waals broadening
Two-parameter van der Waals broadening (Anstee, Barklem & O'Mara, http://www.astro.uu.se/~barklem/howto.html)
Hydrogen lines are computed using Barklem and Piskunov code HLINOP (http://www.astro.uu.se/~barklem/hlinop.html) taking into account self broadening and other effects.
Stark broadening and Stark shift are explicitly computed for the lines of neutral helium.
RTINT
Single pass short-characteristics algorithm
developed for 3D radiative transfer code:
fast and robust even on a sparse grid.
Attenuation operator with quadratic
Bezier spline approximation to the source
function
Bezier spline prevents overshooting
RTINT: equations
RT equation:
Formal solution:
Approximation to the source function:
ππ π‘ β ππ‘2 + ππ‘ + π for ππ β€ π‘ β€ ππ+1
Attenuation operator:
πΌπ+1 = πββπππΌπ + πΌ ππ ππβ1 + π½ππ ππ + πΎππ ππ+1
1
1
1
( )
1
( )
( ) ( )
( )
i i
i
i
i
i i
t
I e I
S t e dt
ππΌπ
ππ= πΌπ β ππ
RTINT: Bezier spline
SME implementation
SME consists of two independent parts: GUI and solver
Solver consists of the IDL routines for preparing spectral synthesis and performing optimization and an external library for computing synthetic spectra
GUI let you prepare data for the solver and interpret the results but there at least two other packages to do it non-interactively
Solver
Spectral synthesis requires various data: line list, wavelength range, atmospheric model(s), initial parameters. All of this (except when model interpolation is required) are collected in one structure β the so-called input structure
Solver takes the input structure and performs its tasks and saves the results into an output structure.
Both input and output structures have name sme
Once the input structure is prepared you can run solver manually: restore,βinput_sme.savβ
sme_main,sme
save,sme,file=βoutput_sme.savβ
Solver
You can also examine the sme structure in your idl session: help,sme,/str
The external library is written in C++ and Fortran and it has about ten entry points.
Conventionally the library should be located in the same place where sme_main.pro is and must be called sme_synth.so. Normally one would create a link with this name to the correct library.
This are used in particular sequence: setting wavelength range, passing atmospheric model, passing line list, solving for molecular-ionization equilibrium, performing spectral synthesis etc.
Things computed within the library with each call are stored in separate memory and can be prompted from IDL using the corresponding calls.
GUI
GUI is interactive tool for creating input structures and examining the output structures
GUI includes tools for importing line lists in VALD format, for importing observations, setting abundances, selecting atmospheric model(s), free parameters etc.
When you save the results of GUI setup, it will automatically create an input structure!
GUI can also read both input and output structures.
GUI also has a graphics tool to show the results.
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