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XMM-Newton spectroscopy of the accreting magnetar candidate 4U0114+65
High Energy Astrophysical Phenomena · Submitted 15 Jun 2017
abstract compiled · 2026-09-23 · no language-model review
The authors' main claim Thus, 4U 0114$+$65 could be a wind-accreting magnetar.
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The abstract, sentence by sentence
4U0114$+$65 is one of the slowest known X-ray pulsars. We present an analysis of a pointed observation by the XMM-Newton X-ray telescope. The energy-resolved light curve, the time-resolved X-ray spectra provided by the EPIC cameras on board and the first high-resolution spectrum of this source, provided by the Reflection Grating Spectrometer, were analysed. An X-ray pulse of $9350\pm 160$ s was measured, confirming the secular spin up of this source. We also fit the pulse-phase-resolved spectra with Comptonisation models. These models imply a very small ($r\sim 3$ km) and hot ($kT\sim 2-3$ keV) emitting region and therefore point to a hot spot over the neutron star (NS) surface as the most reliable explanation for the X-ray pulse. The long NS spin period, the spin-up rate, and persistent X-ray emission can be explained within the theory of quasi-spherical settling accretion, which may indicate that the magnetic field is in the magnetar range. Thus, 4U 0114$+$65 could be a wind-accreting magnetar. We also observed two episodes of low luminosity. The first can be explained as an absorption by an over-dense structure in the wind of the donor. The second episode may be due to temporal cessation of accretion onto one magnetic pole caused by non-spherical matter capture from the structured stellar wind. The light curve displays two types of dips seen during the high-flux intervals. The short dips, with durations of tens of seconds, are produced through absorption by wind clumps. The long dips might be associated with the rarefied interclump medium. We also found evidence of emission lines in the X-ray photoionised wind of the B1Ia donor. The Fe K$\alpha$ line is highly variable and much weaker than in other X-ray binaries with supergiant donors. The degree of wind clumping, measured through the covering fraction, is much lower than in supergiant donor stars with earlier spectral types.
background contribution method result interpretation main claim
| # | sentence | role | the authors' own work | states the main conclusion | strength |
|---|---|---|---|---|---|
| s0 | 4U0114$+$65 is one of the slowest known X-ray pulsars. | background 1.00 | 0.06 | 0.02 | asserted 1.00 |
| s1 | We present an analysis of a pointed observation by the XMM-Newton X-ray telescope. | contribution 0.82 | 0.92 | 0.02 | asserted 0.91 |
| s2 | The energy-resolved light curve, the time-resolved X-ray spectra provided by the EPIC cameras on board and the first high-resolution spectrum of this source, provided by the Reflection Grating Spectrometer, were analysed. | method 0.96 | 0.82 | 0.02 | asserted 0.93 |
| s3 | An X-ray pulse of $9350\pm 160$ s was measured, confirming the secular spin up of this source. | result 1.00 | 0.95 | 0.09 | asserted 1.00 |
| s4 | We also fit the pulse-phase-resolved spectra with Comptonisation models. | method 0.95 | 0.96 | 0.02 | asserted 0.99 |
| s5 | These models imply a very small ($r\sim 3$ km) and hot ($kT\sim 2-3$ keV) emitting region and therefore point to a hot spot over the neutron star (NS) surface as the most reliable explanation for the X-ray pulse. | interpretation 0.99 | 0.90 | 0.18 | hedged possibility 0.64 |
| s6 | The long NS spin period, the spin-up rate, and persistent X-ray emission can be explained within the theory of quasi-spherical settling accretion, which may indicate that the magnetic field is in the magnetar range. | interpretation 1.00 | 0.44 | 0.24 | hedged possibility 0.96 |
| s7 | Thus, 4U 0114$+$65 could be a wind-accreting magnetar. | interpretation 0.99 | 0.43 | 0.57 | hedged possibility 1.00 |
| s8 | We also observed two episodes of low luminosity. | result 0.98 | 0.97 | 0.02 | asserted 1.00 |
| s9 | The first can be explained as an absorption by an over-dense structure in the wind of the donor. | interpretation 0.98 | 0.77 | 0.03 | asserted 0.82 |
| s10 | The second episode may be due to temporal cessation of accretion onto one magnetic pole caused by non-spherical matter capture from the structured stellar wind. | interpretation 0.99 | 0.65 | 0.05 | hedged possibility 0.97 |
| s11 | The light curve displays two types of dips seen during the high-flux intervals. | result 1.00 | 0.88 | 0.02 | asserted 1.00 |
| s12 | The short dips, with durations of tens of seconds, are produced through absorption by wind clumps. | interpretation 0.80 | 0.84 | 0.02 | asserted 1.00 |
| s13 | The long dips might be associated with the rarefied interclump medium. | interpretation 0.96 | 0.76 | 0.03 | speculative 0.98 |
| s14 | We also found evidence of emission lines in the X-ray photoionised wind of the B1Ia donor. | result 1.00 | 0.96 | 0.04 | asserted 0.99 |
| s15 | The Fe K$\alpha$ line is highly variable and much weaker than in other X-ray binaries with supergiant donors. | result 1.00 | 0.89 | 0.03 | asserted 1.00 |
| s16 | The degree of wind clumping, measured through the covering fraction, is much lower than in supergiant donor stars with earlier spectral types. | result 0.99 | 0.93 | 0.04 | asserted 1.00 |
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The paper
Original abstract
4U0114$+$65 is one of the slowest known X-ray pulsars. We present an analysis of a pointed observation by the XMM-Newton X-ray telescope. The energy-resolved light curve, the time-resolved X-ray spectra provided by the EPIC cameras on board and the first high-resolution spectrum of this source, provided by the Reflection Grating Spectrometer, were analysed. An X-ray pulse of $9350\pm 160$ s was measured, confirming the secular spin up of this source. We also fit the pulse-phase-resolved spectra with Comptonisation models. These models imply a very small ($r\sim 3$ km) and hot ($kT\sim 2-3$ keV) emitting region and therefore point to a hot spot over the neutron star (NS) surface as the most reliable explanation for the X-ray pulse. The long NS spin period, the spin-up rate, and persistent X-ray emission can be explained within the theory of quasi-spherical settling accretion, which may indicate that the magnetic field is in the magnetar range. Thus, 4U 0114$+$65 could be a wind-accreting magnetar. We also observed two episodes of low luminosity. The first can be explained as an absorption by an over-dense structure in the wind of the donor. The second episode may be due to temporal cessation of accretion onto one magnetic pole caused by non-spherical matter capture from the structured stellar wind. The light curve displays two types of dips seen during the high-flux intervals. The short dips, with durations of tens of seconds, are produced through absorption by wind clumps. The long dips might be associated with the rarefied interclump medium. We also found evidence of emission lines in the X-ray photoionised wind of the B1Ia donor. The Fe K$\alpha$ line is highly variable and much weaker than in other X-ray binaries with supergiant donors. The degree of wind clumping, measured through the covering fraction, is much lower than in supergiant donor stars with earlier spectral types.
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