A broadband X-ray study of the asynchronous polar: CD Ind

TL;DR

This study presents a detailed broadband X-ray analysis of the asynchronous polar CD Ind, revealing complex absorption, multi-temperature plasma, and spectral variability, leading to insights into the accretion process and white dwarf properties.

Contribution

First broadband X-ray spectral analysis of CD Ind, demonstrating complex absorption, multi-temperature plasma, and spectral variability, advancing understanding of asynchronous polar accretion physics.

Findings

Single broad hump in soft X-ray lightcurve indicates single-pole accretion.

Spectral variability correlates with increased absorption during specific spin phases.

White dwarf mass estimated at approximately 0.87 solar masses.

Abstract

A simultaneous broadband analysis of X-ray data obtained with XMM-Newton and NuSTAR observatories for the asynchronous polar source CD Ind is presented. The spin folded lightcurve in soft 0.3-3.0 keV band shows single broad hump-like structure superimposed with occasional narrow dips, indicating a single-pole accretion model with a complex intrinsic absorber. Lack of strong modulation in folded lightcurve above 3 keV reveals that emission from corresponding zone of post-shock region (PSR) remains in view throughout the spin phase. The broadband spectrum is modelled with a three-component absorbed plasma emission model and absorbed isobaric cooling flow model, both of which fit the data well with similar statistical significance. Presence of partial covering absorber is evident in the spectra with equivalent column density $\sim7\times10^{22}\;\text{cm}^{-2}$ and a covering fraction of $\sim 25\%$. Strong ionised oxygen K$_{\alpha}$ line emission is detected in the spectra. We notice spectral variability during spin phase 0.75-1.05, when there is a considerable increase in column density of overall absorber (from $\sim 1 \times 10^{20}\;\text{cm}^{-2}$ to $\sim 9 \times 10^{20}\;\text{cm}^{-2}$). We required at least three plasma temperatures to describe the multi-temperature nature of the PSR. The shock temperature $\sim 43.3_{-3.4}^{+3.8}$ keV, represented by the upper temperature of the cooling flow model, implies a white dwarf mass of $\sim 0.87^{+0.04}_{-0.03}\;M_{\odot}$. The iron K$_{\alpha}$ line complex shows a strong He-like and a weak neutral fluorescence line. We could not unambiguously detect the presence of Compton reflection in the spectra, which is probably very small and signifying a tall shock height.