X-ray variability of sigma Orionis young stars with ROSAT

TL;DR

This study used ROSAT data to identify X-ray variability in young sigma Orionis stars, revealing that over a third exhibit high-amplitude flares, with variability patterns differing between star types.

Contribution

It is the first to systematically analyze X-ray variability on days-long timescales in sigma Orionis young stars using archival ROSAT data.

Findings

39% of sigma Orionis stars show high-amplitude X-ray variability.

Five stars exhibited clear flares with durations up to six days.

Variability incidence is lower among classical T Tauri stars with disks.

Abstract

We used the Aladin Virtual Obsrvatory tool and High Resolution Imager ROSAT archival data to search for X-ray variability in scale of days in 23 young stars in the sigma Orionis cluster and a background galaxy. Five stars displayed unambiguous flares and had probabilities p_var >> 99% of being actual variables. Two of the detected flares were violent and long-lasting, with maximum duration of six days and amplitude of eight times above the quiescent level. We classified another four stars as possible X-ray variables, including the binary system formed by the B2Vp star sigma Ori E and its close late-type companion. This makes a minimum frequency of high-amplitude X-ray variability in excess of a day of 39% among sigma Orionis stars. The incidence of this kind of X-ray variability seems to be lower among classical T Tauri stars with mid-infrared flux excesses than among fast-rotating, disk-less young stars.