# Variable Hard X-Ray Emission from the Central Star of the Eskimo Nebula

DOI:
10.3847/1538-4357/ab4256
Publication date:
01/10/2019
Main author:
Guerrero, Martín A.
IAA authors:
Guerrero, Martín A.
Authors:
Guerrero, Martín A.;Toalá, Jesús A.;Chu, You-Hua
Journal:
The Astrophysical Journal
Refereed:
Yes
Publication type:
Article
Volume:
884
Pages:
134
Abstract:
The central star of NGC 2392 shows the hardest X-ray emission among central stars of planetary nebulae (CSPNe). The recent discovery of a spectroscopic companion with an orbital period of 1.9 days could provide an explanation for its hard X-ray emission, as well as for the collimation of its fast outflow. Here, we analyze the available Chandra and XMM-Newton X-ray observations to determine accurately the spectral and temporal variation properties of the CSPN of NGC 2392. The X-ray emission can be described by an absorbed thermal plasma model with temperature {26}<SUB>-5</SUB><SUP>+8</SUP> MK and X-ray luminosity (8.7 ± 1.0) × 10<SUP>30</SUP> erg s<SUP>−1</SUP>. No long-term variability is detected in the X-ray emission level, but the Chandra light curve is suggestive of short-term variations with a period ∼0.26 days. The possible origins of this X-ray emission are discussed. X-ray emission from the coronal activity of a companion or shocks in the stellar wind can be ruled out. Accretion of material from an unseen main-sequence companion onto the CSPN or from the CSPN wind onto a white dwarf companion are the most plausible origins for its hard X-ray emission, although the mismatch between the rotational period of the CSPN and the modulation timescale of the X-ray emission seems to preclude the former possibility.
Database: