Deep XMM-Newton observation of the Eta Chamaleontis cluster

TL;DR

This study uses deep XMM-Newton observations to analyze the X-ray properties, variability, and flare activity of stars in the Eta Chamaleontis cluster, revealing correlations with stellar parameters and flare characteristics.

Contribution

It provides the first detailed X-ray analysis of Eta Chamaleontis members, including flare energies and their relation to stellar features, using proprietary deep XMM-Newton data.

Findings

Stars with flares have higher X-ray luminosities than non-flaring stars.

Flare energies are typical of pre-main and main-sequence M stars.

No difference in flare energies between stars with and without disks.

Abstract

The members of the Eta Chamaleontis cluster are in an evolutionary stage in which disks are rapidly evolving. It also presents some peculiarities, such as the large fraction of binaries and accretion disks, probably related with the cluster formation process. Its proximity makes this stellar group an ideal target for studying the relation between X-ray emission and those stellar parameters. The main objective of this work is to determine general X-ray properties of the cluster members in terms of coronal temperature, column density, emission measure, X-ray luminosity and variability. We also aim to establish the relation between the X-ray luminosity of these stars and other stellar parameters, such as binarity and presence of accretion disks. A study of flare energies for each flare event and their relation with some stellar parameters is also performed. We used proprietary data from a deep XMM-Newton observation pointed at the core of the Eta Chamaleontis cluster. Specific software for the reduction of XMM-Newton data was used for the analysis of our observation. For the detection of sources, we used the wavelet-based code PWDetect. General coronal properties were derived from plasma model fitting. We also determined variability of the Eta Chamaleontis members in the EPIC field-of-view. A total of six flare-like events were clearly detected in five different stars. For them, we derived coronal properties during the flare events and pseudo-quiescent state separately. In our observations, stars that underwent a flare event have higher X-ray luminosities in the pseudo-quiescent state than cluster members with similar spectral type with no indications of flaring, independently whether they have an accretion disk or not. Observed flare energies are typical of both pre-main and main-sequence M stars. We detected no difference between flare energies of stars with and without an accretion disk.