Quasi-periodic variation during a fast X-ray outburst of a high-mass X-ray binary MAXI J0709-159 / LY CMa observed by NICER

TL;DR

This paper reports the discovery of a quasi-periodic oscillation at 1.1 Hz during a fast X-ray outburst of the high-mass X-ray binary MAXI J0709-159, providing insights into the accretion process and magnetic field of the neutron star.

Contribution

The study presents the first detection of a QPO during a short outburst of a supergiant fast X-ray transient, linking it to the neutron star's magnetic field and accretion dynamics.

Findings

Detected a 1.1 Hz QPO during the outburst.

Estimated the neutron star's magnetic field to be ~10^12 G.

Observed rapid variability and spectral changes consistent with clumpy wind accretion.

Abstract

We report on a quasi-periodic variation at $\sim1$ Hz during a fast X-ray outburst of a high-mass X-ray binary MAXI J0709$-$159 / LY CMa observed by the Neutron-star interior composition explorer (NICER). The new X-ray transient MAXI J0709$-$159 was discovered on 2022 January 25. Due to the transient X-ray behavior characterized by the short (a few hours) outburst duration, rapid ($\lesssim$ 1 s) variability with spectral change, and large luminosity swing from $10^{32}$ erg s$^{-1}$ to $10^{37}$ erg s$^{-1}$, the object was considered likely to be a supergiant X-ray binary with a neutron star (NS) categorized as a Supergiant Fast X-ray Transient (SFXT). Follow-up NICER and NuSTAR observations confirmed that the position of the new X-ray object is consistent with a Be star, LY CMa, which has been also identified as a B supergiant. We analyzed the NICER data obtained from 3 hours to 6 days after the discovery. The light curve reveals that the X-ray activity continued for $\sim7$ hours in sparse short flares, each lasting $\lesssim 100$ seconds, and the luminosity instantaneously reached up to $\sim 1\times 10^{38}$ erg s$^{-1}$. The light-curve and spectral features reasonably agree with those expected from accretion of a clumpy stellar-wind onto a magnetized NS. The variability power spectrum during the brightest flare shows a broad peak at $1.1$ Hz resembling a quasi-periodic oscillation (QPO). If the QPO is attributed to the Keplerian orbital frequency at the inner edge of a transient accretion disk truncated by the NS magnetosphere, the NS surface magnetic field is estimated to be $\sim 10^{12}$ G.