Non-thermal radio emission in Sakurai's Object

TL;DR

This study tracks nearly two decades of radio emissions from Sakurai's Object, revealing shock-induced non-thermal emission initially, followed by thermal emission likely caused by star-driven photoionization, thus constraining its reheating timeline.

Contribution

It provides the first long-term radio monitoring of Sakurai's Object, distinguishing between shock and photoionization phases to better understand VLTP evolution.

Findings

Non-thermal emission from shocks observed from 2004 to 2017.

Transition to thermal emission indicating photoionization since 2019.

Flux density fluctuated significantly over months to years.

Abstract

The very late thermal pulse (VLTP) affects the evolution of $\sim$20\% of 1--8\,$\mathrm M_\odot$ stars, repeating the last phases of the red giant within a few years and leading to the formation of a new, but hydrogen-poor nebula within the old planetary nebula (PN). The strong dust formation in the latter obscures the optical and near-infrared radiation of the star. We aimed to determine the reheating timescale of the central star in Sakurai's object, which is an important constraint for the poorly understood VLTP evolution. We observed the radio continuum emission of Sakurai's object for almost 20 years from 2004 to 2023. Continuous, multi-frequency observations proved to be essential to distinguish between phases dominated by photoionization and shock ionization. The flux density fluctuates by more than a factor 40 within months to years. The spectral index remained negative between 2006 and 2017 and is close to zero since 2019. The emission region is barely resolved since 2021. Non-thermal radio emission observed from 2004 to 2017 traces shocks induced by wind interactions due to discrete mass-loss events. Thermal emission dominates during the period 2019--2023 and may indicate photoionization of the nebula by the central star.