SRGA J124404.1–632232/SRGU J124403.8–632231: New X-ray pulsar discovered in the all-sky survey by the SRG

Doroshenko, V.; Staubert, R.; Maitra, Chandreyee; Rau, A.; Haberl, F.; Santangelo, A.; Schwope, A. D.; Wilms, J.; Buckley, D.; Semena, A.; Mereminskiy, I. A.; Lutovinov, A.; Gromadzki, M.; Townsend, L. J.; Monageng, I. M.

doi:10.1051/0004-6361/202141147

Cited by 7 publications

(2 citation statements)

References 39 publications

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“…This allowed us to perform a detailed spectral analysis and to compare the spectral shape at very different mass-accretion rates. The goal of this was to verify our assumption of strong changes in the spectra in XRPs when their luminosity reaches ∼10 35 erg s −1 as was recently found in several X-ray pulsars (X Persei, Doroshenko et al 2012;GX 304−1, Tsygankov et al 2019c Doroshenko et al 2022). These spectral changes manifest themselves in the transformation of the classical pulsar-like into a double-hump spectrum and were shown to be caused by the Comptonisation of cyclotron photons in the upper overheated layer of the neutron star atmosphere (Mushtukov et al 2021;Sokolova-Lapa et al 2021).…”

Section: Spectral Evolutionsupporting

confidence: 51%

SRG/ART-XC, Swift, NICER, and NuSTAR study of different states of the transient X-ray pulsar MAXI J0903–531

Tsygankov

Molkov

Doroshenko

et al. 2022

A&A

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The results of the broadband spectral and timing study of the recently discovered transient X-ray pulsar MAXI J0903–531 in a wide range of luminosities that differ by a factor of ~30 are reported. The observed X-ray spectrum in both states can be described as a classical pulsar-like spectrum consisting of a power law with a high-energy cutoff. We argue that the absence of the spectrum transformation to the two-hump structure that is expected at low fluxes indicates that the magnetic field of the neutron star is relatively weak below (2–3) × 1012 G. This estimate is consistent with other indirect constraints and non-detection of any absorption features that might be interpreted as a cyclotron absorption line. The timing analysis of the NuSTAR data revealed only slight variations of a single-peaked pulse profile of the source as a function of the energy band and mass accretion rate. In both intensity states, the pulsed fraction increases from 40% to roughly 80% with the energy. Finally, we were also able to obtain the orbital solution for the binary system using data from the Fermi/GBM, NICER, and NuSTAR instruments.

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Section: Spectral Evolutionsupporting

confidence: 51%

SRG/ART-XC, Swift, NICER, and NuSTAR study of different states of the transient X-ray pulsar MAXI J0903–531

Tsygankov

Molkov

Doroshenko

et al. 2022

A&A

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“…This capability is crucial for systems which have never been observed at high-luminosity states, that is, for which cyclotron lines have never been observed in the spectra. This class of Be X-ray binaries accreting in quiescence is actively growing, e.g., through NuSTAR follow-up of Be X-ray binary candidates found during the first eROSITA All Sky Survey [see, e.g., Doroshenko et al (2022)]. More similar discoveries are expected as deeper X-ray survey data from eROSITA become available.…”

Section: Constraining the Surface Magnetic Field Strength From Quiesc...mentioning

confidence: 97%

The high energy X-ray probe (HEX-P): a new window into neutron star accretion

Ludlam,

Malacaria,

Sokolova-Lapa

et al. 2023

Front. Astron. Space Sci.

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Accreting neutron stars (NSs) represent a unique laboratory for probing the physics of accretion in the presence of strong magnetic fields (B ≳ 108 G). Additionally, the matter inside the NS itself exists in an ultra-dense, cold state that cannot be reproduced in Earth-based laboratories. Hence, observational studies of these objects are a way to probe the most extreme physical regimes. Here we present an overview of the field and discuss the most important outstanding problems related to NS accretion. We show how these open questions regarding accreting NSs in both low-mass and high-mass X-ray binary systems can be addressed with the High-Energy X-ray Probe (HEX-P) via simulated data. In particular, with the broad X-ray passband and improved sensitivity afforded by a low X-ray background, HEX-P will be able to 1) distinguish between competing continuum emission models; 2) provide tighter upper limits on NS radii via reflection modeling techniques that are independent and complementary to other existing methods; 3) constrain magnetic field geometry, plasma parameters, and accretion column emission patterns by characterizing fundamental and harmonic cyclotron lines and exploring their behavior with pulse phase; 4) directly measure the surface magnetic field strength of highly magnetized NSs at the lowest accretion luminosities; as well as 5) detect cyclotron line features in extragalactic sources and probe their dependence on luminosity in the super-Eddington regime in order to distinguish between geometrical evolution and accretion-induced decay of the magnetic field. In these ways HEX-P will provide an essential new tool for exploring the physics of NSs, their magnetic fields, and the physics of extreme accretion.

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SRG/ART-XC discovery of SRGA J204318.2+443815: Towards the complete population of faint X-ray pulsars

Lutovinov

Tsygankov

Mereminskiy

et al. 2022

A&A

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We report a discovery of a new long-period X-ray pulsar SRGA J204318.2+443815/SRGe J204319.0+443820 in the Be binary system. The source was found in the second all-sky survey by the Mikhail Pavlinsky ART-XC telescope on board the SRG mission. The follow-up observations with XMM-Newton, NICER and NuSTAR observatories allowed us to discover a strong coherent signal in the source light curve with the period of ∼ 742 s. The pulsed fraction was found to depend on the energy increasing from ∼ 20% in soft X-rays to > 50% at high energies, as it is typical for X-ray pulsars. The source demonstrate a quite hard spectrum with an exponential cutoff at high energies and bolometric luminosity of L X 4 × 10 35 erg s −1 . Dedicated optical and infrared observations with the RTT-150, NOT, Keck and Palomar telescopes revealed a number of emission lines (H α , He i, Pashen and Braket series) with the strongly absorbed continuum. All of above suggests that SRGA J204318.2+443815/SRGe J204319.0+443820 is a new persistent low luminosity X-ray pulsar in a distant binary system with a Be-star of the B0-B2e class. Thus the SRG observatory allow us to unveil the hidden population of faint persistent objects including the population of slowly rotating X-ray pulsars in Be systems.

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SRGA J124404.1–632232/SRGU J124403.8–632231: New X-ray pulsar discovered in the all-sky survey by the SRG

Cited by 7 publications

References 39 publications

SRG/ART-XC, Swift, NICER, and NuSTAR study of different states of the transient X-ray pulsar MAXI J0903–531

SRG/ART-XC, Swift, NICER, and NuSTAR study of different states of the transient X-ray pulsar MAXI J0903–531

The high energy X-ray probe (HEX-P): a new window into neutron star accretion

SRG/ART-XC discovery of SRGA J204318.2+443815: Towards the complete population of faint X-ray pulsars

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