An application of the Ghosh &amp; Lamb model to the accretion-powered X-ray pulsar X Persei

Yatabe, F.; Makishima, Kazuo; Mihara, T.; Nakajima, M.; Sugizaki, M.; Kitamoto, Shunji; Yoshida, Yuki; Takagi, T.

doi:10.1093/pasj/psy088

Cited by 18 publications

(29 citation statements)

References 44 publications

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“…In the case of wind-capture accretion in supergiant high-mass X-ray binaries, Corbet & Krimm (2013) discussed the relation between their modulation and the geometry of binary systems and determined that the superorbital period is proportional to the binary orbital period. In contrast, as claimed by Yatabe et al (2018), X Per has a disk accretion scheme similar to that of the other Be/X-ray binaries. Thus, the variation of the mass-transfer rate from a circumstellar disc to a neutron star is the cause of the periodic superorbital modulation.…”

Section: Discussionmentioning

confidence: 75%

“…X Persei (X Per or 4U 0352+309) is a classical persistent Be/X-ray binary composed of a slowly rotating X-ray pulsar (P spin ∼ 835 second; Yatabe et al 2018) and (09.5III-B0Ve) optical companion (HD 24534;Lyubimkov et al 1997). This source was independently discovered by Ariel 5 and Copernicus (White et al 1976).…”

Section: Long-term X-ray and Optical Variationsmentioning

confidence: 99%

“…Since the pulse-phase resolved spectroscopy results and the orbital modulation of X Per have already been discussed in several papers (e.g. Lutovinov et al 2012; 7-year X-ray periodicity from X Persei Maitra et al 2017;Yatabe et al 2018), our analysis is focused on X-ray spectrum variability in superorbital modulation. We utilized the 2-20 keV data obtained by the MAXI/GSC (MJD 55058-58331) which covers 1.3 superorbital cycles.…”

Section: X-ray Spectral Analysismentioning

confidence: 99%

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Firm detection of 7-year X-ray periodicity from X Persei

Nakajima¹,

Negoro

Mihara

et al. 2018

Proc. IAU

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We report on the detection of long-term X-ray periodicity from the Be/X-ray binary pulsar X Persei. Based on over 23 years of X-ray data observed using RXTE/ASM, Swift/BAT and MAXI/GSC, we confirmed that X Persei exhibits quasi-periodic X-ray flares with a period of ∼7 years. The recurrence timescale corresponds to approximately 10 times its binary orbital period of 250 days. Spectral and hardness ratio changes were not detected along with long-term periodic activity. If we interpret the observed 7 year periodicity of X-ray band flux as a superorbital modulation, then this would be the first observation among the Be/X-ray binaries.

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Section: Discussionmentioning

confidence: 75%

Section: Long-term X-ray and Optical Variationsmentioning

confidence: 99%

Section: X-ray Spectral Analysismentioning

confidence: 99%

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Firm detection of 7-year X-ray periodicity from X Persei

Nakajima¹,

Negoro

Mihara

et al. 2018

Proc. IAU

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“…Accurate estimates of the surface MF of accreting NSs are available through detections of cyclotron resonance scattering features (CRSFs) in their X-ray spectra (Makishima 2016). However, the current observational sensitivity limits the CRSF detections to < ∼ 100 keV, and hence B < ∼ 10 13 G. As an alternative method to estimate the dipole component of B (particularly towards higher values) of accreting NSs, the classical accretion torque theory by Ghosh and Lamb (1979), hereafter GL79, has been revived, calibrated, and applied to several high-mass X-ray binaries (HMXBs) (Takagi et al 2016;Makishima 2016;Sugizaki et al 2017;Yatabe et al 2018;Sugizaki et al 2020). In particular, Yatabe et al (2018) studied X Persei, the HMXB which has an NS companion with a long spin period (∼835 s) in an approximate torque equilibrium, a low luminosity (∼10 35 erg s −1 ), and a hard continuum extending to ∼ 80 keV without a clear cutoff.…”

Section: Introductionmentioning

confidence: 99%

“…However, the current observational sensitivity limits the CRSF detections to < ∼ 100 keV, and hence B < ∼ 10 13 G. As an alternative method to estimate the dipole component of B (particularly towards higher values) of accreting NSs, the classical accretion torque theory by Ghosh and Lamb (1979), hereafter GL79, has been revived, calibrated, and applied to several high-mass X-ray binaries (HMXBs) (Takagi et al 2016;Makishima 2016;Sugizaki et al 2017;Yatabe et al 2018;Sugizaki et al 2020). In particular, Yatabe et al (2018) studied X Persei, the HMXB which has an NS companion with a long spin period (∼835 s) in an approximate torque equilibrium, a low luminosity (∼10 35 erg s −1 ), and a hard continuum extending to ∼ 80 keV without a clear cutoff. The application of the GL79 modeling has shown that the NS in X Persei has B ∼10 14 G, which is significantly higher than those of ordinary X-ray pulsars, and is comparable to those of magnetars.…”

Section: Introductionmentioning

confidence: 99%

A study of the accretion mechanisms of the High Mass X-ray Binary IGR J00370+6122

Uchida,

Takahashi,

Fukazawa

et al. 2021

Preprint

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IGR J00370+6122 is a high-mass X-ray binary, of which the primary is a B1 Ib star, whereas the companion is suggested to be a neutron star by the detection of 346-s pulsation in one-off 4-ks observation. To better understand the nature of the compact companion, the present work performs timing and spectral studies of the X-ray data of this object, taken with XMM-Newton, Swift, Suzaku, RXTE, and INTEGRAL. In the XMM-Newton data, a sign of coherent 674 s pulsation was detected, for which the previous 346-s period may be the 2nd harmonic.The spectra exhibited the "harder when brighter" trend in the 1-10 keV range, and a flat continuum without clear cutoff in the 10-80 keV range. These properties are both similar to those observed from several low-luminosity accreting pulsars, including X Persei in particular. Thus, the compact object in IGR J00370+6122 is considered to be a magnetized neutron star with a rather low luminosity. The orbital period was refined to 15.6649 ± 0.0014 d. Along the orbit, the luminosity changes by 3 orders of magnitude, involving a sudden drop from ∼ 4 × 10 33 to ∼ 1 × 10 32 erg s −1 at an orbital phase of 0.3 (and probably vice verse at 0.95). Although these phenomena cannot be explained by a simple Hoyle-Lyttleton accretion from the primary's stellar winds, they can be explained when incorporating the propeller effect with a strong dipole 1 magnetic field of ∼ 5 × 10 13 G. Therefore, the neutron star in IGR J00370+6122 may have a stronger magnetic field compared to ordinary X-ray pulsars.

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Optical spectroscopy of the Be/black hole binary MWC 656 ‐ interaction of a black hole with a circumstellar disc

et al. 2022

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We present new spectroscopic observations of the Be/black hole binary MWC 656 obtained during the period 2015–2021. We measure the equivalent width of Hα (EWα), Hβ (EWβ$$ {EW}_{\beta } $$), and the distance between the peaks of Hα (normalΔVα$$ \Delta {V}_{\alpha } $$), Hβ (normalΔVβ$$ \Delta {V}_{\beta } $$), and FeII (normalΔVFeII$$ \Delta {V}_{\mathrm{FeII}} $$) lines. Combining new and old data, we find that: (1) the density of the circumstellar disc of MWC 656 (normalΔVα$$ \Delta {V}_{\alpha } $$ versus EWα$$ {EW}_{\alpha } $$ diagram) is similar to the Be stars. For the Be stars, we find the relation normalΔVβ=0.999normalΔVα+62.4$$ \Delta {V}_{\beta }=0.999\Delta {V}_{\alpha }+62.4 $$ km s−1, and the position of MWC 656 corresponds to the average behavior of the Be stars. This means that the presence of the black hole does not change the overall structure of the circumstellar disc; (2) the periodogram analysis indicates modulation of EWα$$ {EW}_{\alpha } $$ with a period 60.4±0.4$$ 60.4\pm 0.4 $$ days, which is identical to the binary orbital period. The maxima of EWα$$ {EW}_{\alpha } $$ and EWβ$$ {EW}_{\beta } $$ are around periastron (phase zero); (3) around orbital phase zero, normalΔVβ$$ \Delta {V}_{\beta } $$ and normalΔVFeII$$ \Delta {V}_{FeII} $$ decrease by about 30$$ 30 $$ km s−1. This suggests that we observe an increase of the circumstellar disc size induced by the periastron passage of the black hole and that the entire circumstellar disc pulsates with the orbital period with relative amplitude of 10–20%. The observations also indicate, that the reason for the black hole in MWC 656 to be in deep quiescence is a very low efficiency of accretion (∼2×10−6$$ \sim 2\times {10}^{-6} $$).

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An application of the Ghosh & Lamb model to the accretion-powered X-ray pulsar X Persei

Cited by 18 publications

References 44 publications

Firm detection of 7-year X-ray periodicity from X Persei

Firm detection of 7-year X-ray periodicity from X Persei

A study of the accretion mechanisms of the High Mass X-ray Binary IGR J00370+6122

Optical spectroscopy of the Be/black hole binary MWC 656 ‐ interaction of a black hole with a circumstellar disc

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