A detailed X-ray investigation of zeta Puppis - The variability on short and long timescales

TL;DR

This study analyzes X-ray data of zeta Puppis to investigate its wind variability, revealing a slow flux modulation possibly linked to corotating regions and placing new constraints on wind clumping in massive stars.

Contribution

It provides the first constraints on the number of wind clumps in an O-type star using X-ray observations, highlighting the high fragmentation of stellar winds.

Findings

Detected a slow X-ray flux modulation with up to 15% amplitude.

No significant short-term variability was observed, only consistent with Poisson noise.

Constrained the wind to have over 10^5 clumps, indicating high wind fragmentation.

Abstract

Stellar winds are a crucial component of massive stars, but their exact properties still remain uncertain. To shed some light on this subject, we have analyzed an exceptional set of X-ray observations of zeya Pup, one of the closest and brightest massive stars. The sensitive lightcurves that were derived reveal two major results. On the one hand, a slow modulation of the X-ray flux (with a relative amplitude of up to 15% over 16h in the 0.3--4.0keV band) is detected. Its characteristic timescale cannot be determined with precision, but amounts from one to several days. It could be related to corotating interaction regions, known to exist in zeta Pup from UV observations. Hour-long changes, linked to flares or to the pulsation activity, are not observed in the last decade covered by the XMM observations; the 17h tentative period, previously reported in a ROSAT analysis, is not confirmed either and is thus transient, at best. On the other hand, short-term changes are surprisingly small (<1% relative amplitude for the total energy band). In fact, they are compatible solely with the presence of Poisson noise in the data. This surprisingly low level of short-term variability, in view of the embedded wind-shock origin, requires a very high fragmentation of the stellar wind, for both absorbing and emitting features (>10^5 parcels, comparing with a 2D wind model). This is the first time that constraints have been placed on the number of clumps in an O-type star wind and from X-ray observations.