Doppler Imaging of Stellar Magnetic Field

Doppler reconstruction of the stellar magnetic field distribution. The upper two rows of spherical plots (a, b) show the true magnetic map, the lower rows (c, d) present reconstruction from the simulated observations in four Stokes parameters. No external constraints on the field geometry were imposed. In each pair of rows the first plot (a, c) shows surface map of the field strength and the second row (b, d) illustrates the field orientation. The length of the arrows is proportional to the local field strength. The red arrows show field vectors pointing outside the stellar surface and the blue arrows correspond to the vectors pointing inwards.
Kochukhov & Piskunov, 2002, A&A, 388, 868
Magnetic Doppler imaging of the surface field in the bright chemically peculiar A star α2 CVn (a: field strength, b: field orientation). This magnetic map was recovered self-consistently with chemical inhomogeneities using high-resolution observations in the Stokes I and V parameters.
Kochukhov et al., 2002, A&A, 389, 420
Magnetic Doppler imaging of the surface field in the famous chemically peculiar star 53 Cam (a: field strength, b: field orientation). For the first time magnetic geometry in an early-type star is inferred using high-resolution spectra in all four Stokes parameters and without assuming a low-order multipolar parameterization of the stellar field geometry. Our magnetic Doppler image of 53 Cam reveals unexpected complexity of the field in this star, urging significant reevalution of the basic facts and theories of stellar magnetism.
Kochukhov et al., 2004, A&A, 414, 613
Magnetic Doppler imaging of the very young (9 Myr) chemically peculiar B-type star HD 72106. Magnetic map (a: field strength, b: field orientation) was derived from observations in the Stokes I and V parameters. HD 72106 is a member of a binary system with Herbig Ae star. Its strong, global magnetic field and prominent surface chemical inhomogeneities show that magnetic CP-star phenomenon can develop in B-type stars very quickly after the star is born.
Folsom, Wade, Kochukhov, et al., 2008, MNRAS, 391, 901