The Nature of the Hard-X-Ray Emitting Symbiotic Star RT Cru

TL;DR

This study presents Chandra observations of RT Cru, a symbiotic star with a white dwarf emitting hard X-rays beyond 50 keV, revealing a cooling flow spectrum and accretion disk characteristics without magnetic channelling evidence.

Contribution

First detailed X-ray spectral analysis of RT Cru, identifying its accretion disk boundary layer and confirming the white dwarf's mass and non-magnetic accretion nature.

Findings

X-ray spectrum consistent with an isobaric cooling flow

Detection of rapid stochastic variability below 4 keV

No evidence of magnetic channelling or pulsations

Abstract

We describe Chandra High-Energy Transmission Grating Spectrometer observations of RT Cru, the first of a new sub-class of symbiotic stars that appear to contain white dwarfs (WDs) capable of producing hard X-ray emission out to greater than 50 keV. The production of such hard X-ray emission from the objects in this sub-class (which also includes CD -57 3057, T CrB, and CH Cyg) challenges our understanding of accreting WDs. We find that the 0.3 -- 8.0 keV X-ray spectrum of RT Cru emanates from an isobaric cooling flow, as in the optically thin accretion-disk boundary layers of some dwarf novae. The parameters of the spectral fit confirm that the compact accretor is a WD, and they are consistent with the WD being massive. We detect rapid, stochastic variability from the X-ray emission below 4 keV. The combination of flickering variability and a cooling-flow spectrum indicates that RT Cru is likely powered by accretion through a disk. Whereas the cataclysmic variable stars with the hardest X-ray emission are typically magnetic accretors with X-ray flux modulated at the WD spin period, we find that the X-ray emission from RT Cru is not pulsed. RT Cru therefore shows no evidence for magnetically channeled accretion, consistent with our interpretation that the Chandra spectrum arises from an accretion-disk boundary layer.