Discovery of Quasi Periodic Oscillations in the persistent X-ray emission of Accreting Binary X-ray Pulsar LMC X-4

TL;DR

This paper reports the first detection of quasi-periodic oscillations in the persistent X-ray emission of the pulsar LMC X-4, providing new insights into the accretion processes and magnetic field estimation of the neutron star.

Contribution

It presents the discovery of QPOs in the persistent emission of LMC X-4, a novel observation that enhances understanding of accretion dynamics in high magnetic field neutron star systems.

Findings

QPOs detected at 20-30 mHz in persistent emission

First observation of QPOs in LMC X-4's persistent state

Estimated magnetic field strength of the neutron star

Abstract

We report the discovery of quasi-periodic oscillations (QPOs) in the High Mass X-ray Binary (HMXB) pulsar LMC X-4 in its non-flaring (persistent) state using observations with XMM-Newton. In addition to the 74 mHz coherent pulsations, the persistent emission light curve shows a QPO feature in the frequency range of 20-30 mHz. Quasi-periodic flares have been previously observed from LMC X-4 in observations made with Rossi X-ray Timing Explorer (RXTE). However, this is the first time QPOs have been observed in the persistent emission observations of LMC X-4. QPOs in X-ray binaries are generally thought to be related to the rotation of the inhomogeneous matter distribution in the inner accretion disk. In High Mass X-ray Binaries (HMXBs) such as LMC X-4 where the compact object is a neutron star with a high magnetic field, the radius of the inner accretion disk is determined by the mass accretion rate and the magnetic moment of the neutron star. In such systems, the QPO feature, along with the pulse period and X-ray luminosity measurement helps us to constrain the magnetic field strength of the neutron star. We use considerations of magnetospheric accretion to have an approximate value of the magnetic field strength of the neutron star in LMC X-4.