The X-Ray Pulsar XTE J1858+034 Observed with NuSTAR and Fermi/GBM: Spectral and Timing Characterization plus a Cyclotron Line
Wilms J; Malacaria C; Jenke P; Lutovinov Alexander A.; Wilson-Hodge CA; Coley Joel B.; Pottschmidt K; Tsygankov Sergey S.; Kretschmar P; Madsen KK
The X-Ray Pulsar XTE J1858+034 Observed with NuSTAR and Fermi/GBM: Spectral and Timing Characterization plus a Cyclotron Line
Wilms J
Malacaria C
Jenke P
Lutovinov Alexander A.
Wilson-Hodge CA
Coley Joel B.
Pottschmidt K
Tsygankov Sergey S.
Kretschmar P
Madsen KK
IOP PUBLISHING LTD
Julkaisun pysyvä osoite on:
https://urn.fi/URN:NBN:fi-fe2021042827334
https://urn.fi/URN:NBN:fi-fe2021042827334
Tiivistelmä
Accreting X-ray pulsars (XRPs) undergo luminous X-ray outbursts during
which the spectral and timing behavior of the neutron star can be
studied in detail. We analyze a NuSTAR observation of the XRP XTE
J1858+034 during its outburst in 2019. The spectrum is fit with a
phenomenological, a semiempirical, and a physical spectral model. A
candidate cyclotron line is found at 48 keV, implying a magnetic field
of 5.4 × 1012 G at the site of emission. This is also
supported by the physical best-fit model. We propose an orbital period
of about 81 days based on the visual inspection of the X-ray outburst
recurrence time. Based on Fermi/GBM data, the standard disk
accretion-torque theory allowed us to infer a distance of 10.9 ± 1.0
kpc. Pulse profiles are single-peaked and show a pulsed fraction that is
strongly energy-dependent at least up to 40 keV.
which the spectral and timing behavior of the neutron star can be
studied in detail. We analyze a NuSTAR observation of the XRP XTE
J1858+034 during its outburst in 2019. The spectrum is fit with a
phenomenological, a semiempirical, and a physical spectral model. A
candidate cyclotron line is found at 48 keV, implying a magnetic field
of 5.4 × 1012 G at the site of emission. This is also
supported by the physical best-fit model. We propose an orbital period
of about 81 days based on the visual inspection of the X-ray outburst
recurrence time. Based on Fermi/GBM data, the standard disk
accretion-torque theory allowed us to infer a distance of 10.9 ± 1.0
kpc. Pulse profiles are single-peaked and show a pulsed fraction that is
strongly energy-dependent at least up to 40 keV.
Kokoelmat
- Rinnakkaistallenteet [19207]