lte-codes	sterne	spectrum	ffit	sfit	grids	idlines
commands

STERNE

C.S. Jeffery, D. Schönberner, U. Heber, 1974-2002

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LTE line-blanketed model atmospheres for hot stars

Plane-parallel line-blanketed model atmospheres for hot stars, Teff>8000K, in local thermal, radiative and hydrostatic equilibrium. Atomic bound-free opacities are treated as in ATLAS, supplemented by additional tables for C, C+, C++, C+++, N, N+, N++, N+++ (Peach 1970). Line opacities are treated using odf's as in ATLAS6. The code handles extremely H-deficient mixtures and composition stratification. A grid of model atmospheres computed using Sterne is available.

Invocation

Sterne [control [odf [interval [model] ] ] ]

control	file containing parameters for required model
odf	file containing opacity distribution function
interval	frequency interval for wavelengths: BIG or LIT
model	file containing starting model

The contents of the file control is described in the reference guide. If control is omitted, information not provided on the command line will be requested by the script. Output files are constructed by appending a label to the string control.

Additional Commands

Sterne.input Teff logg nH nHe nC nN grey datfile

Sets up a file datfile containing the required model parameters and which may be used as the input file control.

Sterne.final datfile odf

Takes the output from sterne stored in datfile and computes final model using a LIT interval opacity distribution function odf.

sterne_qub

Formats output for use with DIPSO and spectrum.

Example

Sterne.input 20000 4.0 0.9 0.1 0.004 0.006 0 lte2040
Sterne lte2040 dfbp00 BIG
Sterne.final lte2040 dflp00

Versions

Sterne.2

Sterne.2.4 (Default)

Sterne.2.5

A new version developed by Paul Harrison and Simon Jeffery (St Andrew and Armagh) includes provision for

• new photo-ionization cross-sections from the Opacity Project,
• more extensive line opacities

The OP opacities are still being tested, and the opacity sampling code is still under development.

Sterne.3

Another version developed by Paul Harrison (St Andrews and Armagh) includes a more stable and faster temperature correction procedure, and a completely rebuilt internal structure. This is not yet operational.

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This page is maintained by:
Simon Jeffery (csj@star.arm.ac.uk)
Last modified: 02-Jun-2003