Confirmation of the presence of a CRSF in the NICER spectrum of X 1822-371
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arXiv
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2024
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| author | Iaria, R. Di Salvo, T. Anitra, A. Miceli, C. Barra, F. Leone, W. Burderi, L. Sanna, A. Riggio, A. |
| author_facet | Iaria, R. Di Salvo, T. Anitra, A. Miceli, C. Barra, F. Leone, W. Burderi, L. Sanna, A. Riggio, A. |
| contents | X 1822-371 is an eclipsing binary system with a period close to 5.57 hr and an orbital period derivative $\dot{P}_{\rm orb}$ of 1.42(3)$\times 10^{-10}$ s s$^{-1}$. The extremely high value of its $\dot{P}_{\rm orb}$ is compatible with a super-Eddington mass transfer rate from the companion star and, consequently, an intrinsic luminosity at the Eddington limit. The source is also an X-ray pulsar, it shows a spin frequency of 1.69 Hz and is in a spin-up phase with a spin frequency derivative of $7.4 \times 10^{-12}$ Hz s$^{-1}$. Assuming a luminosity at the Eddington limit, a neutron star magnetic field strength of $B = 8 \times 10^{10}$ G is estimated. However, a direct measure of $B$ could be obtained observing a CRSF in the energy spectrum. Analysis of \textit{XMM-Newton} data suggested the presence of a cyclotron line at 0.73 keV, with an estimated magnetic field strength of $B=(8.8 \pm 0.3) \times 10^{10}$ G. Here we analyze the 0.3-50 keV broadband spectrum of X 1822-371 combining a 0.3-10 keV NICER spectrum and a 4.5-50 keV \textit{NuSTAR} spectrum to investigate the presence of a cyclotron absorption line and the complex continuum emission spectrum. The NICER spectrum confirms the presence of a cyclotron line at 0.66 keV. The continuum emission is modeled with a Comptonized component, a thermal component associated with the presence of an accretion disk truncated at the magnetospheric radius of 105 km and a reflection component from the disk blurred by relativistic effects. We confirm the presence of a cyclotron line at 0.66 keV inferring a NS magnetic field of $B = (7.9\pm 0.5) \times 10^{10}$ G and suggesting that the Comptonized component originates in the accretion columns. |
| format | Preprint |
| id |
arxiv_https___arxiv_org_abs_2401_03698 |
| institution | arXiv |
| publishDate | 2024 |
| record_format | arxiv |
| spellingShingle | Confirmation of the presence of a CRSF in the NICER spectrum of X 1822-371 Iaria, R. Di Salvo, T. Anitra, A. Miceli, C. Barra, F. Leone, W. Burderi, L. Sanna, A. Riggio, A. High Energy Astrophysical Phenomena X 1822-371 is an eclipsing binary system with a period close to 5.57 hr and an orbital period derivative $\dot{P}_{\rm orb}$ of 1.42(3)$\times 10^{-10}$ s s$^{-1}$. The extremely high value of its $\dot{P}_{\rm orb}$ is compatible with a super-Eddington mass transfer rate from the companion star and, consequently, an intrinsic luminosity at the Eddington limit. The source is also an X-ray pulsar, it shows a spin frequency of 1.69 Hz and is in a spin-up phase with a spin frequency derivative of $7.4 \times 10^{-12}$ Hz s$^{-1}$. Assuming a luminosity at the Eddington limit, a neutron star magnetic field strength of $B = 8 \times 10^{10}$ G is estimated. However, a direct measure of $B$ could be obtained observing a CRSF in the energy spectrum. Analysis of \textit{XMM-Newton} data suggested the presence of a cyclotron line at 0.73 keV, with an estimated magnetic field strength of $B=(8.8 \pm 0.3) \times 10^{10}$ G. Here we analyze the 0.3-50 keV broadband spectrum of X 1822-371 combining a 0.3-10 keV NICER spectrum and a 4.5-50 keV \textit{NuSTAR} spectrum to investigate the presence of a cyclotron absorption line and the complex continuum emission spectrum. The NICER spectrum confirms the presence of a cyclotron line at 0.66 keV. The continuum emission is modeled with a Comptonized component, a thermal component associated with the presence of an accretion disk truncated at the magnetospheric radius of 105 km and a reflection component from the disk blurred by relativistic effects. We confirm the presence of a cyclotron line at 0.66 keV inferring a NS magnetic field of $B = (7.9\pm 0.5) \times 10^{10}$ G and suggesting that the Comptonized component originates in the accretion columns. |
| title | Confirmation of the presence of a CRSF in the NICER spectrum of X 1822-371 |
| topic | High Energy Astrophysical Phenomena |
| url | https://arxiv.org/abs/2401.03698 |