X-ray emission from the M9 dwarf 1RXS J115928.5-524717 - Quasi-quiescent coronal activity at the end of the main sequence

TL;DR

This study reports the detection of quasi-quiescent X-ray emission from the ultracool M9 dwarf 1RXS J115928.5-524717, revealing persistent coronal activity similar to more massive stars despite different internal structures.

Contribution

First detailed analysis of X-ray emission from an M9 ultracool dwarf showing persistent coronal activity, indicating efficient magnetic dynamo mechanisms at the end of the main sequence.

Findings

Detected X-ray emission at L_x ≈ 1.0 x 10^26 erg/s

Coronal plasma modeled with two temperatures: 2 MK and 6 MK

X-ray activity level of log L_x/L_bol = -4.1

Abstract

Methods: We analyse an XMM-Newton observation of 1RXS J115928.5-524717, an ultracool dwarf with spectral type M9 and compare its X-ray properties to those of other similar very late-type stars. Results: We clearly detected 1RXS J115928.5-524717 at soft X-ray energies in all EPIC detectors. Only minor variability was present during the observation and we attribute the X-ray emission to quasi-quiescent activity. The coronal plasma is described well by a two-temperature model at solar metallicity with temperatures of 2 MK and 6 MK and an X-ray luminosity of about L_x = 1.0 x 10^26 erg/s in the 0.2-2.0 keV band. The corresponding activity level of log L_x/L_bol = -4.1 points to a moderately active star. Altogether, X-ray activity from very low-mass stars shows similar trends to more massive stars, despite their different interior structure. 1RXSJ115928.5-524717 is, after LHS 2065, the second ultracool M9 dwarf that emits X-rays at detectable levels in quasi-quiescence. While faint in absolute numbers,both stars are rather X-ray active, implying the existence of an efficient dynamo mechanisms that is capable of creating magnetic activity and coronal X-ray emission.