TY - JOUR

T1 - First characterization of a new high-mass X-ray binary in LMC eRASSU J050810.4-660653 with SRG/ART-XC, NuSTAR, and Swift

AU - Salganik, Alexander

AU - Tsygankov, Sergey S.

AU - Lutovinov, Alexander A.

AU - Mushtukov, Alexander A.

AU - Mereminskiy, Ilya A.

AU - Molkov, Sergey V.

AU - Semena, Andrei N.

N1 - Publisher Copyright: © 2022 The Author(s) Published by Oxford University Press on behalf of Royal Astronomical Society.

PY - 2022/8/1

Y1 - 2022/8/1

N2 - We report results of the first detailed spectral and temporal studies of the recently discovered Be/X-ray binary eRASSU J050810.4-660653 in Large Magellanic Cloud based on the data from the SRG/ART-XC, NuSTAR and Swift/XRT instruments obtained in 2021 December-2022 May in a wide energy range of 0.5-79 keV. Pulsations with the period of 40.5781 ± 0.0004 s were found in the source light curve with the pulsed fraction monotonically increasing with the energy. An estimate of the orbital period of ?38 d was obtained based on the long-Term monitoring of the system. The source spectrum can be well approximated with a power-law model modified by an exponential cutoff at high energies. The pulse phase-resolved spectroscopy shows a strong variation of spectral parameters depending on the phase of a neutron star rotation. We have not found any features connected with the cyclotron absorption line both in the phase-Averaged and phase-resolved spectra of eRASSU J050810.4-660653. However, the neutron star magnetic field was estimated around several 1013 G using different indirect methods. Discovered variations of the hardness ratio over the pulse phase is discussed in terms of physical and geometrical properties of the emitting region.

AB - We report results of the first detailed spectral and temporal studies of the recently discovered Be/X-ray binary eRASSU J050810.4-660653 in Large Magellanic Cloud based on the data from the SRG/ART-XC, NuSTAR and Swift/XRT instruments obtained in 2021 December-2022 May in a wide energy range of 0.5-79 keV. Pulsations with the period of 40.5781 ± 0.0004 s were found in the source light curve with the pulsed fraction monotonically increasing with the energy. An estimate of the orbital period of ?38 d was obtained based on the long-Term monitoring of the system. The source spectrum can be well approximated with a power-law model modified by an exponential cutoff at high energies. The pulse phase-resolved spectroscopy shows a strong variation of spectral parameters depending on the phase of a neutron star rotation. We have not found any features connected with the cyclotron absorption line both in the phase-Averaged and phase-resolved spectra of eRASSU J050810.4-660653. However, the neutron star magnetic field was estimated around several 1013 G using different indirect methods. Discovered variations of the hardness ratio over the pulse phase is discussed in terms of physical and geometrical properties of the emitting region.

KW - accretion, accretion discs

KW - pulsars: general

KW - scattering

KW - stars: magnetic field

KW - stars: neutron

KW - X-rays: binaries

UR - http://www.scopus.com/inward/record.url?scp=85133808802&partnerID=8YFLogxK

UR - https://www.mendeley.com/catalogue/1180fb1a-c378-3394-804d-25175c0ada5b/

U2 - 10.1093/mnras/stac1608

DO - 10.1093/mnras/stac1608

M3 - Article

AN - SCOPUS:85133808802

VL - 514

SP - 4018

EP - 4025

JO - Monthly Notices of the Royal Astronomical Society

JF - Monthly Notices of the Royal Astronomical Society

SN - 0035-8711

IS - 3

ER -