Zeeman–Doppler imaging

Surface magnetic field of SU Aur (a young star of T Tauri type), reconstructed by means of Zeeman–Doppler Imaging

In astrophysics, Zeeman–Doppler imaging is a tomographic technique dedicated to the cartography of stellar magnetic fields, as well as surface brightness and temperature distributions.

This method makes use of the ability of magnetic fields to polarize the light emitted (or absorbed) in spectral lines formed in the stellar atmosphere (the Zeeman effect). The periodic modulation of Zeeman signatures during the stellar rotation is employed to make an iterative reconstruction of the vectorial magnetic field at stellar surface.

The method was first proposed by Marsh and Horne in 1988, as a way to interpret the emission line variations of cataclysmic variable stars.[1] This techniques is based on the principle of maximum entropy image reconstruction; it yields the simplest magnetic field geometry (as a spherical harmonics expansion) among the various solutions compatible with the data.[2]

This technique is the first to enable the reconstruction of the vectorial magnetic geometry of stars similar to the Sun. It is now offering the opportunity to undertake systematic studies of stellar magnetism and is also yielding information on the geometry of large arches that magnetic fields are able to develop above stellar surfaces. To collect the observations related to Zeeman-Doppler Imaging, astronomers use stellar spectropolarimeters like ESPaDOnS [3] at CFHT on Mauna Kea (Hawaii), HARPSpol [4] at the ESO's 3.6m telescope (La Silla Observatory, Chile), as well as NARVAL[5] at Bernard Lyot Telescope (Pic du Midi de Bigorre, France).

The technique is very reliable, as the reconstruction of the magnetic field maps with different algorithms yield almost identical results, even with poorly sampled data sets.[6]

References

  1. ↑ Marsh, T. R.; Horne, K. (1 November 1988). "Images of accretion discs - II. Doppler tomography". Monthly Notices of the Royal Astronomical Society. 235 (1): 269–286. Bibcode:1988MNRAS.235..269M. doi:10.1093/mnras/235.1.269.
  2. ↑ Donati, J.-F.; Howarth, I. D.; Jardine, M. M.; Petit, P.; et al. (2006). "The surprising magnetic topology of τ Sco: fossil remnant or dynamo output?". Monthly Notices of the Royal Astronomical Society. 370 (2): 629–644. arXiv:astro-ph/0606156Freely accessible. Bibcode:2006MNRAS.370..629D. doi:10.1111/j.1365-2966.2006.10558.x.
  3. ↑ ESPaDOnS
  4. ↑ http://www.astro.uu.se/~piskunov/RESEARCH/INSTRUMENTS/HARPSpol/
  5. ↑ NARVAL
  6. ↑ Hussain, G. A. J.; Donati, J.- F.; Collier Cameron, A.; Barnes, J. R. (11 November 2000). "Comparisons of images derived from independent Zeeman Doppler imaging codes". Monthly Notices of the Royal Astronomical Society. 318 (4): 961–973. Bibcode:2000MNRAS.318..961H. doi:10.1046/j.1365-8711.2000.03573.x.

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