Jet creation in post-AGB binaries: the circum-companion accretion disc around BD+46$^{\circ}$442

TL;DR

This study analyzes the origin and properties of high-velocity jets in the post-AGB binary BD+46°442, revealing a gaseous accretion disk around the companion star as the jet source, using spectral analysis and Doppler tomography.

Contribution

It provides the first detailed modeling and imaging of the accretion disk and jet in BD+46°442, demonstrating the binary interaction's role in jet formation in post-AGB systems.

Findings

High-velocity outflows are linked to an accretion disk around the secondary.

Jet velocities exceed 400 km/s.

The outflow has a wide opening angle, not strongly collimated.

Abstract

We aim at describing and understanding binary interaction processes in systems with very evolved companions. Here, we focus on understanding the origin and determining the properties of the high-velocity outflow observed in one such system. We present a quantitative analysis of BD+46$^{\circ}$442, a post-AGB binary which shows active mass transfer that leads to the creation of a disk-driven outflow or jet. We obtained high-resolution optical spectra from the HERMES spectrograph, mounted on the 1.2m Flemish Mercator Telescope. By performing a time-series analysis of the Halpha profile, we dissected the different components of the system. We deduced the jet geometry by comparing the orbital phased data with our jet model. In order to image the accretion disk around the companion of BD+46$^{\circ}$442, we applied the technique of Doppler tomography. The orbital phase-dependent variations in the Halpha profile can be related to an accretion disk around the companion, from which a high-velocity outflow or jet is launched. Our model shows that there is a clear correlation between the inclination angle and the jet opening angle. The latitudinally dependent velocity structure of our jet model shows a good correspondence to the data, with outflow velocities at least higher than 400km/s. We show that BD+46$^{\circ}$442, is a result of a binary interaction channel. The origin of the fast outflow in this system can be attributed to a gaseous disk around the secondary component, which is most likely a main sequence star. Our analysis suggests the outflow to have a rather wide opening angle instead of being strongly collimated. Similar orbital phase-dependent Halpha profiles are commonly observed in post-AGB binaries. Post-AGB binaries provide ideal test bets to study jet formation and launching mechanisms over a wide range of orbital conditions.