4U 1538-52 in a Heartbeat: Broadband X-ray Spectral Properties from XMM-Newton and NuSTAR
Abstract
Context. Galactic high-mass X-ray binaries (HMXBs) are important systems for studying accretion mechanisms onto compact objects and for investigating the complex stellar winds of massive stars. In particular, HMXBs that host a neutron star allow us to reveal the structure of the accreted material in X-ray pulsars and consequently to investigate how matter behaves under extreme conditions of pressure and density. These are major scientific goals for XRISM and NewAthena . Aims. Here we report on the first out-of-eclipse XMM-Newton observation of the HMXB 4U 1538−52, complemented by NuSTAR coverage. Our campaign aimed to investigate stellar-wind variability and continuum changes with high-resolution spectroscopy at a critical orbital phase: when the neutron star is in inferior conjunction. Methods. Thanks to simultaneous observations covering both soft and hard X-rays, we obtain the most detailed X-ray view of the accreted material in 4U 1538−52 to date. In particular, we perform time-resolved spectroscopy down to the pulse period of the neutron star to highlight wind clumping properties and accretion structures. Results. In this dataset, we observe a bright flare reaching ∼10 37 erg s −1 probably induced by the accretion of a 10 20 g clump, followed by a luminosity dip forming a heartbeat-like episode. This event is followed by three local absorption peaks with local variability of the order of the pulse period and a gradual hardening of the underlying spectrum throughout the observation. This could indicate the presence of both small-scale and large-scale overdense structures in the vicinity of the neutron star, which can be attributed to clumps and filamentary structures embedded in the accretion wake. These observational evidences are further supported and reproduced by 3D hydrodynamic simulations.
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BibTeX
@article{diez2026153852,
title = {{4U 1538-52 in a Heartbeat: Broadband X-ray Spectral Properties from XMM-Newton and NuSTAR}},
author = {C.M Diez and S Dupourqué and A.-L Doherty and D Dickson and A Zainab and S Martínez-Núñez and J.M Torrejón and S Guillot and A. Rouco Escorial and F Fürst and P Kretschmar},
journal = {Astron.Astrophys.},
year = {2026},
month = sep,
doi = {10.1051/0004-6361/202661853},
eprint = {2608.14938},
archivePrefix = {arXiv},
url = {https://hal.science/hal-05758453v1},
note = {CC BY},
}
RIS
TY - JOUR
TI - 4U 1538-52 in a Heartbeat: Broadband X-ray Spectral Properties from XMM-Newton and NuSTAR
AU - C.M Diez
AU - S Dupourqué
AU - A.-L Doherty
AU - D Dickson
AU - A Zainab
AU - S Martínez-Núñez
AU - J.M Torrejón
AU - S Guillot
AU - A. Rouco Escorial
AU - F Fürst
AU - P Kretschmar
PY - 2026
DA - 2026/09/22
JO - Astron.Astrophys.
DO - 10.1051/0004-6361/202661853
UR - https://hal.science/hal-05758453v1
AB - Context. Galactic high-mass X-ray binaries (HMXBs) are important systems for studying accretion mechanisms onto compact objects and for investigating the complex stellar winds of massive stars. In particular, HMXBs that host a neutron star allow us to reveal the structure of the accreted material in X-ray pulsars and consequently to investigate how matter behaves under extreme conditions of pressure and density. These are major scientific goals for XRISM and NewAthena . Aims. Here we report on the first out-of-eclipse XMM-Newton observation of the HMXB 4U 1538−52, complemented by NuSTAR coverage. Our campaign aimed to investigate stellar-wind variability and continuum changes with high-resolution spectroscopy at a critical orbital phase: when the neutron star is in inferior conjunction. Methods. Thanks to simultaneous observations covering both soft and hard X-rays, we obtain the most detailed X-ray view of the accreted material in 4U 1538−52 to date. In particular, we perform time-resolved spectroscopy down to the pulse period of the neutron star to highlight wind clumping properties and accretion structures. Results. In this dataset, we observe a bright flare reaching ∼10 37 erg s −1 probably induced by the accretion of a 10 20 g clump, followed by a luminosity dip forming a heartbeat-like episode. This event is followed by three local absorption peaks with local variability of the order of the pulse period and a gradual hardening of the underlying spectrum throughout the observation. This could indicate the presence of both small-scale and large-scale overdense structures in the vicinity of the neutron star, which can be attributed to clumps and filamentary structures embedded in the accretion wake. These observational evidences are further supported and reproduced by 3D hydrodynamic simulations.
ER -