Magnetospheric accretion on the T Tauri star BP Tauri

TL;DR

This study uses spectropolarimetric observations to map the magnetic topology and accretion spots of the T Tauri star BP Tauri, revealing a complex magnetic field likely generated by dynamo action, influencing its accretion processes and rotation.

Contribution

First detailed magnetic topology reconstruction of BP Tauri showing a mainly-axisymmetric poloidal field generated by dynamo action in a fully-convective star.

Findings

BP Tau has a 1.2 kG dipole and 1.6 kG octupole magnetic field.

Accretion spots are located at high latitudes, covering about 2% of the stellar surface.

Magnetosphere extends at least 4 stellar radii, coupling with the accretion disc near the corotation radius.

Abstract

From observations collected with the ESPaDOnS and NARVAL spectropolarimeters, we report the detection of Zeeman signatures on the classical T Tauri star BP Tau. Circular polarisation signatures in photospheric lines and in narrow emission lines tracing magnetospheric accretion are monitored throughout most of the rotation cycle of BP Tau at two different epochs in 2006. We observe that rotational modulation dominates the temporal variations of both unpolarised and circularly polarised spectral proxies tracing the photosphere and the footpoints of accretion funnels. From the complete data sets at each epoch, we reconstruct the large-scale magnetic topology and the location of accretion spots at the surface of BP Tau using tomographic imaging. We find that the field of BP Tau involves a 1.2 kG dipole and 1.6 kG octupole, both slightly tilted with respect to the rotation axis. Accretion spots coincide with the two main magnetic poles at high latitudes and overlap with dark photospheric spots; they cover about 2% of the stellar surface. The strong mainly-axisymmetric poloidal field of BP Tau is very reminiscent of magnetic topologies of fully-convective dwarfs. It suggests that magnetic fields of fully-convective cTTSs such as BP Tau are likely not fossil remants, but rather result from vigorous dynamo action operating within the bulk of their convective zones. Preliminary modelling suggests that the magnetosphere of BP Tau extends to distances of at least 4 R* to ensure that accretion spots are located at high latitudes, and is not blown open close to the surface by a putative stellar wind. It apparently succeeds in coupling to the accretion disc as far out as the corotation radius, and could possibly explain the slow rotation of BP Tau.