Complex structure of the magnetic field of the CP-Star HD142301

Abstract

Models of the magnetic field of the He-w star HD142301 are constructed. Observational data are well described by the model of a dipole shifted by 0.6 stellar radii transverse to the axis. The phase dependence of the HeI λ4026Å line, however, corresponds better to a model assuming the presence of four monopoles (or two dipoles) shifted by 0.4 stellar radii from the center. The distance between the monopoles in both models is comparable to the star's radius, which indicates that the source of the magnetic field is "long" dipoles, rather than "point" dipoles.

The polarization mode of the auroral radio emission from the early-type star HD 142301

“…The comparison between the observed and the simulated auroral pulses allows us also to confirm the suspected non-dipolar nature of the magnetic field topology of HD 142301 as suggested by Glagolevskij (2010). For a dipole shaped ORM, the auroral pulses coincide with the phases where the magnetic dipole axis is located in the plane of the sky (null effective magnetic field).…”

“…Consequently, the polar field strength of HD 142301, estimated by using the Eq. 1, is B p = 14100 G. However, a field topology more complex than a simple dipole has been proposed to describe the magnetic field of HD 142301 (Glagolevskij 2010).…”

The fifth main-sequence magnetic B-type star showing coherent radio emission: Is this really a rare phenomenon?

“…In the case of σ Ori E, the absence of ECME was attributed to the presence of a strong quadrupolar component (Leto et al 2012). Interestingly, none of the 5 magnetic stars with ECME has been found to have an ideal dipolar magnetic field (e.g., Kochukhov et al 2014Kochukhov et al , 2017Shultz et al 2018;Leto et al 2019;Glagolevskij 2010). Thus, to solve the problem of when ECME can be stimulated, it will be important to have a precise constraints on the surface magnetic topology via Zeeman Doppler Imaging (e.g.…”