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Doppler and Zeeman Doppler Imaging of Stars

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Cartography of the Sun and the Stars

Part of the book series: Lecture Notes in Physics ((LNP,volume 914))

Abstract

In this chapter we discuss the problem of reconstructing two-dimensional stellar surface maps from the variability of intensity and/or polarisation profiles of spectral lines. We start by outlining the main principles of the scalar Doppler imaging problem concerned with recovering maps of chemical spots, temperature or brightness from the intensity spectra. After presenting the physical and mathematical foundations of this remote sensing method, we review its applications to mapping different types of spots in early-type chemically peculiar and late-type active stars, and non-radial pulsations in early-type stars. We also discuss an extension of Doppler imaging to the problem of recovering vector distributions of stellar magnetic fields from spectropolarimetric observations and review applications of this Zeeman Doppler imaging technique in the context of stellar magnetism studies.

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Notes

  1. 1.

    We refer to the textbook by Landi Degl’Innocenti and Landolfi (2004) for a comprehensive review of spectral line polarisation theory.

  2. 2.

    Somewhat confusingly, such ZDI with the spherical harmonic regularisation is still commonly called “maximum entropy” inversion although the employed regularisation is quite different from the original MEM-based ZDI scheme described by Brown et al. (1991).

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  1. Department of Physics and Astronomy, Uppsala University, Box 516, SE 75120, Uppsala, Sweden

    Oleg Kochukhov

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  1. Oleg Kochukhov
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Correspondence to Oleg Kochukhov .

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  1. Observatoire de la Côte d'Azur, Nice, France

    Jean-Pierre Rozelot

  2. Observatoire de Paris-Meudon, Meudon, France

    Coralie Neiner

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Kochukhov, O. (2016). Doppler and Zeeman Doppler Imaging of Stars. In: Rozelot, JP., Neiner, C. (eds) Cartography of the Sun and the Stars. Lecture Notes in Physics, vol 914. Springer, Cham. https://doi.org/10.1007/978-3-319-24151-7_9

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