J/A+A/374/265 LTE spectrum synthesis in magnetic atmospheres (Wade+, 2001)
LTE spectrum synthesis in magnetic stellar atmospheres.
The interagreement of three independent polarised radiative transfer codes.
Wade G.A., Bagnulo S., Kochukhov O., Landstreet J.D., Piskunov N.,
Stift M.J.
<Astron. Astrophys. 374, 265 (2001)>
=2001A&A...374..265W 2001A&A...374..265W
ADC_Keywords: Models, atmosphere ; Magnetic fields ; Line Profiles ;
Polarization
Keywords: masers - polarization, line profiles, stars: magnetic fields
Description:
Files table4.dat contain calculated Stokes IQUV local line profiles of
Fe II 4923.9 shown in Fig. 4 of this paper. Profile sets are provided
for 0.1, 5 and 20kG magnetic fields, with vector orientation
ψ=40°, φ=0°, disc centre and epsfe=4.6.
File Summary:
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FileName Lrecl Records Explanations
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ReadMe 80 . This file
table4a.dat 138 4731 List of monochromatic intensities vs wavelength
0.1kG (10mT) field
table4b.dat 138 4731 List of monochromatic intensities vs wavelength
5kG (0.5T) field
table4c.dat 138 4731 List of monochromatic intensities vs wavelength
20kG (2T) field
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See also:
http://fedelma.astro.univie.ac.at/web/cossam/index.html : COSSAM home page
Byte-by-byte Description of file: table4?.dat
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Bytes Format Units Label Explanations
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1- 10 F10.4 0.1nm lambda Wavelength in angstroms
13- 22 F10.6 --- CossamI Stokes I normalised monochromatic intensity,
calculated by Cossam (1)
23- 32 F10.6 --- CossamQ Stokes Q normalised monochromatic intensity,
calculated by Cossam (1)
33- 42 F10.6 --- CossamU Stokes U normalised monochromatic intensity,
calculated by Cossam (1)
43- 52 F10.6 --- CossamV Stokes V normalised monochromatic intensity,
calculated by Cossam (1)
56- 65 F10.6 --- Invers10I Stokes I normalised monochromatic intensity,
calculates by Invers10 (2)
66- 75 F10.6 --- Invers10Q Stokes Q normalised monochromatic intensity,
calculated by Invers10 (2)
76- 85 F10.6 --- Invers10U Stokes U normalised monochromatic intensity,
calculated by Invers10 (2)
86- 95 F10.6 --- Invers10V Stokes V normalised monochromatic intensity,
calculated by Invers10 (2)
99-108 F10.6 --- Zeeman2I Stokes I normalised monochromatic intensity,
calculated by Zeeman2 (3)
109-118 F10.6 --- Zeeman2Q ? Stokes Q normalised monochromatic intensity,
calculated by Zeeman2 (3)
119-128 F10.6 --- Zeeman2U ? Stokes U normalised monochromatic intensity,
calculated by Zeeman2 (3)
129-138 F10.6 --- Zeeman2V ? Stokes V normalised monochromatic intensity,
calculated by Zeeman2 (3)
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Note (1): COSSAM stands for
"Codice per la sintesi spettrale nelle atmosfere magnetiche".
It is the first object-oriented parallel code in the field of
(polarised) spectral line synthesis and is the result of a major
software engineering effort. COSSAM is designed for the accurate
direct calculation of full Stokes IQUV spectra in the sun or in
rotating and/or pulsating stars whose magnetic fields are represented
by a tilted, eccentric dipole, or by a dipole-quadrupole expansion.
Source code, data files and documentation can be downloaded from:
http://fedelma.astro.univie.ac.at/web/cossam/index.html
Note (2): INVERS10 is a Magnetic Doppler Imaging code designed for
reconstructing the distribution of magnetic field vectors and
abundance of one chemical element over the surface of magnetic Ap
stars. The maps are recovered from a time series of the
spectropolarimetric observations by solving a regularised inverse
problem.
Note (3): ZEEMAN2 is the descendant of the original FORTRAN-77 LTE
line synthesis code ZEEMAN, described by Landstreet
(1988ApJ...326..967L 1988ApJ...326..967L). The code is designed both for direct
calculation of polarised spectra and for modeling of data using a
simple field description and a simply parametrised element
distribution.
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Acknowledgements: Gregg A. Wade
(End) Gregg A. Wade [Universite de Montreal], Patricia Bauer [CDS] 20-Aug-2001