Spin-Down of the Long-Period Accreting Pulsar 4u 2206+54

Finger, Mark H.; Ikhsanov, N. R.; Wilson-Hodge, C.; Patel, S.

doi:10.1088/0004-637x/709/2/1249

Cited by 38 publications

(61 citation statements)

References 31 publications

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“…Some models predict the system 4U 2206+543 to harbour a magnetar (see, e.g. Finger et al, 2010). In addition to the spectral model typical for X-ray pulsars (power law with high energy cut-off), some evidence of a cyclotron resonance scattering feature at energies ∼ 30 and ∼ 60 keV were presented using RXTE, BeppoSAX (Torrejón et al, 2004), and INTEGRAL (Blay et al, 2005;Wang, 2009) data.…”

Section: High-mass X-ray Binaries In the Milky Way 71mentioning

confidence: 99%

High-mass X-ray binaries in the Milky Way

Walter

Lutovinov

Bozzo

et al. 2015

Astron Astrophys Rev

234

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High-mass X-ray binaries are fundamental in the study of stellar evolution, nucleosynthesis, structure and evolution of galaxies and accretion processes. Hard X-rays observations by INTEGRAL and Swift have broadened significantly our understanding in particular for the super-giant systems in the Milky Way, which number has increased by almost a factor of three. INTEGRAL played a crucial role in the discovery, study and understanding of heavily obscured systems and of fast X-ray transients. Most super-giant systems can now be classified in three categories: classical/obscured, eccentric and fast transient.The classical systems feature low eccentricity and variability factor of ∼ 10 3 , mostly driven by hydrodynamic phenomena occurring on scales larger than the accretion radius. Among them, systems with short orbital periods and close to Roche-Lobe overflow or with slow winds, appear highly obscured. In eccentric systems, the variability amplitude can reach even higher factors, because of the contrast of the wind density along the orbit. Four super-giant systems, featuring fast outbursts, very short orbital periods and anomalously low accretion rates, are not yet understood.Simulations of the accretion processes on relatively large scales have progressed and reproduce parts of the observations. The combined effects of wind

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Section: High-mass X-ray Binaries In the Milky Way 71mentioning

confidence: 99%

High-mass X-ray binaries in the Milky Way

Walter

Lutovinov

Bozzo

et al. 2015

Astron Astrophys Rev

234

View full text Add to dashboard Cite

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“…For instance, Finger et al (2010) interpreted 4U 2206+54 (P s ∼ 5560 s) as an accreting magnetar. Efforts to explain the long period pulsars by alternative models are accumulating: Ikhsanov (2007) incorporated a subsonic propeller state into the evolutionary tracks of NSs, which can overcome the spin period barrier of ∼ 500 s; Wang & Chang (2012) proposed a retrograde wind accretion to explain long spin periods of supergiant fast X-ray transients (see also Christodoulou et al 2017); suggested a magnetized accretion stream to explain the long spin period of 4U 2206+54 where the magnetic field at the surface of the NS is expected to be ∼4×10 12 G; Shakura et al (2012Shakura et al ( , 2013 developed a model for quasi-spherical subsonic accretion, which can explain long spin periods of the NSs in symbiotic XRBs.…”

Section: See Section 43)mentioning

confidence: 99%

Deep Chandra Survey of the Small Magellanic Cloud. II. Timing Analysis of X-Ray Pulsars

Hong

Antoniou

Zezas

et al. 2017

ApJ

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We report the timing analysis results of X-ray pulsars from a recent deep Chandra survey of the Small Magellanic Cloud (SMC). We have analyzed a total exposure of 1.4 Ms from 31 observations over a 1.2 deg 2 region in the SMC under a Chandra X-ray Visionary Program. Using the Lomb-Scargle and epoch folding techniques, we have detected periodic modulations from 20 pulsars and a new candidate pulsar. The survey also covers 11 other pulsars with no clear sign of periodic modulation. The 0.5-8 keV X-ray luminosity (L X ) of the pulsars ranges from 10 34 to 10 37 erg s −1 at 60 kpc. All the Chandra sources with L X 4×10 35 erg s −1 exhibit X-ray pulsations. The X-ray spectra of the SMC pulsars (and high mass X-ray binaries) are in general harder than those of the SMC field population. All but SXP 8.02 can be fitted by an absorbed power-law model with a photon index of Γ 1.5. The X-ray spectrum of the known magnetar SXP 8.02 is better fitted with a two-temperature blackbody model. Newly measured pulsation periods of SXP 51.0, SXP 214 and SXP 701 are significantly different from the previous XMM-Newton and RXTE measurements. This survey provides a rich data set for energy-dependent pulse profile modeling. Six pulsars show an almost eclipse-like dip in the pulse profile. Phase-resolved spectral analysis reveals diverse spectral variation during pulsation cycle: e.g., for an absorbed power-law model, some exhibit an (anti)-correlation between absorption and X-ray flux, while others show more intrinsic spectral variation (i.e., changes in photon indices).

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“…However, there are some metallic lines typical for a later-type spectrum (Negueruela & Reig 2001). The compact object is a neutron star (Torrejón et al 2004) with spin period P s = 5554±9 s (Finger et al 2010). The X-ray spectrum of 4U 2206+54 is typical for a neutron star accreting material onto its magnetic poles.…”

Section: U 2206+54 (Bd 53mentioning

confidence: 99%

Orbital parameters of the high‐mass X‐ray binary 4U 2206+54

et al. 2014

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We present new radial velocities of the high-mass X-ray binary star 4U 2206+54 based on optical spectra obtained with the Coudé spectrograph at the 2m RCC telescope at the Rozhen National Astronomical Observatory, Bulgaria in the period November 2011 -July 2013 . The radial velocity curve of the HeI λ6678Å line is modeled with an orbital period P orb = 9.568 d and an eccentricity of e = 0.3. These new measurements of the radial velocity resolve the disagreements of the orbital period discussions.

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Spin-Down of the Long-Period Accreting Pulsar 4u 2206+54

Cited by 38 publications

References 31 publications

High-mass X-ray binaries in the Milky Way

High-mass X-ray binaries in the Milky Way

Deep Chandra Survey of the Small Magellanic Cloud. II. Timing Analysis of X-Ray Pulsars

Orbital parameters of the high‐mass X‐ray binary 4U 2206+54

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