Three-Dimensional Doppler Tomography of the RS Vulpeculae Interacting Binary

TL;DR

This study uses 3D Doppler tomography to analyze Hα emission in RS Vulpeculae, revealing magnetic activity-induced gas flows at high velocities, differing from typical gravitational flow patterns.

Contribution

First application of 3D Doppler tomography to RS Vul, uncovering magnetic activity effects on gas flow not seen in previous 2D studies.

Findings

Revealed high-velocity gas streams at Vz = -240 to -360 km/s

Detected magnetic activity influencing gas flow

Identified differences from U CrB's streamlike state

Abstract

Three-dimensional Doppler tomography has been used to study the H$\alpha$ emission sources in the RS Vulpeculae interacting binary. The 2D tomogram of this binary suggested that most of the emission arose from the cool mass losing star with additional evidence of gas flowing close to the predicted trajectory. However, the 3D tomogram revealed surprising evidence of a more pronounced gas stream flow at high $V_z$ velocities from -240 to -360 km s{$^{-1}$}. This behavior is most likely caused by magnetic activity on the cool star since the central velocity plane, defined by $V_z$ = 0 km s{$^{-1}$}, should be coincident with the orbital plane of the binary if the flow is dominated by gravitational forces only. RS Vul has been detected as both an X-ray and a radio source, and it is possible that the RS Vul gas stream may have been deflected by magnetic field lines. This flow is distinctly different from that found in the streamlike state of U CrB, in which the gas flow was confined mostly to the central velocity plane.