The onset of photoionization in Sakurai's Object (V4334 Sgr)

TL;DR

This study tracks the evolution of Sakurai's Object, revealing the onset of photoionization around 2005 through radio and optical observations, and discusses implications for stellar evolution and mass ejection.

Contribution

It provides the first evidence of photoionization onset in Sakurai's Object using radio and optical data, updating previous shock-based interpretations.

Findings

Radio flux increased sharply between 2005 and 2006.

Optical emission lines faded due to post-shock cooling.

Stellar temperature increased to 12 kK in 2006.

Abstract

We investigate the reheating of the very late thermal pulse (VLTP) object V4334 Sgr (Sakurai's Object) using radio observations from the Very Large Array, and optical spectra obtained with the Very Large Telescope. We find a sudden rise of the radio flux at 5 and 8 GHz - from <= 90 micro-Jy and 80 +/- 30 micro-Jy in February 2005 to 320 micro-Jy and 280 micro-Jy in June 2006. Optical line emission is also evolving, but the emission lines are fading. The optical line emission and early radio flux are attributed to a fast shock (and not photoionization as was reported earlier) which occurred around 1998. The fading is due to post-shock cooling and recombination. The recent rapid increase in radio flux is evidence for the onset of photoionization of carbon starting around 2005. The current results indicate an increase in the stellar temperature to 12 kK in 2006. The mass ejected in the VLTP eruption is M_ej >= 1e-4 Msol, but could be as high as 1e-2 Msol, depending mainly on the distance and the clumping factor of the outflow. We derive a distance between 1.8 and 5 kpc. A high mass loss could expose the helium layer and yield abundances compatible with those of [WC] and PG1159 stars.