Doppler Imaging of stellar magnetic fields. I. Techniques

By N. Piskunov, O. Kochukhov. 2002

160 citations recorded by the source corpus.

Subfields: Astronomy and Astrophysics

View Paper: https://www.semanticscholar.org/paper/01f0965be253309513627791c0262c4790876c90

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In Astronomy and Astrophysics

1. A. Reiners
2. J. Donati
3. N. Piskunov
4. J. Landstreet
5. J. Valenti
6. O. Kochukhov
7. V. Makaganiuk
8. P. Petit

Citations in the corpus

• Stable magnetic fields in stellar interiors (2005, unknown): “A more sophisticated approach which can yield better results is that of Zeeman-Doppler Imaging (see Piskunov & Kochukhov 2002), which has as of yet only been applied to a very small number of stars, owing to the high quality of the spectra required.”
• Least-squares deconvolution of the stellar intensity and polarization spectra (2010, background): “Figure 2 in Piskunov & Kochukhov (2002) illustrates the definitio of these angles.”
• Magnetic Fields of Nondegenerate Stars (2009, methodology): “A variation of ZDI, called Magnetic Doppler Imaging (Piskunov & Kochukhov 2002), also aims at mapping magnetic fields on stellar surfaces from setsof time-resolved Zeeman signatures, incorporating polarised radiative transfer in the reconstruction process.”
• Dynamo processes and activity cycles of the active stars AB Doradus, LQ Hydrae and HR 1099 (2003, background): “…circumstances; pairs of low-latitude magnetic field belts of opposite polarities encircling the star and located symmetrically about the equator belong to this category, remaining easily undetected in circular polarization at stellar inclination angles close to 90◦ (Piskunov & Kochukhov 2002).”
• Observations of Cool-Star Magnetic Fields (2012, methodology): “An example from Piskunov and Kochukhov (2002) is shown in Figure 6, another one from Donati (2001) is reproduced in Figure 7, and a third example from Donati and Brown (1997) is shown in Figure 8.”
• Spectroscopy Made Easy: Evolution (2016, methodology): “A quadratic fit to the source function makes this solver comparable with or superior to the Feautrier method (see Piskunov & Kochukhov 2002, Fig.”