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