Cygnus X-1 - Polarization evidence for an extended secondary envelope with an eclipsing region

Kemp, J. C.; Barbour, M. S.; Parker, Timothy E.; Herman, L. C.

doi:10.1086/182895

Cited by 19 publications

(9 citation statements)

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“…We use this to deduce that Larwood’s model fits our data if we assume i =20°. This is rather low (e.g., Bruevich et al 1978 suggest i =40°–60° and Kemp et al 1979 suggest i =60°–70°), and so it appears that some refinement to the model is necessary.…”

Section: Resultsmentioning

confidence: 99%

Orbital, precessional and flaring variability of Cygnus X-1

Brocksopp¹,

Fender²,

Larionov³

et al. 1999

Monthly Notices of the Royal Astronomical Society

150

197

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We present the results of a 2.5-year multiwavelength monitoring programme of Cygnus X-1, making use of hard and soft X-ray data, optical spectroscopy, UBVJHK photometry and radio data. In particular we confirm that the 5.6-day orbital period is apparent in all wavebands and note the existence of a wavelength-dependence to the modulation, in the sense that higher energies reach minimum first. We also find a strong modulation at a period of 142 ± 7 days, which we suggest is due to precession and/or radiative warping of the accretion disc. Strong modulation of the hard and soft X-ray flux at this long period may not be compatible with simple models of an optically thin accretion flow and corona in the low state. We present the basic components required for more detailed future modelling of the system-including a partially optically thick jet, quasi-continuous in the low state, the base of which acts as the Comptonising corona. In addition, we find that there are a number of flares which appear to be correlated in at least two wavebands and generally in more. We choose two of these flares to study in further detail and find that the hard and soft X-rays are well-correlated in the first and that the soft X-rays and radio are correlated in the second. In general, the optical and infrared show similar behaviour to each other but are not correlated with the X-rays or radio.

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Section: Resultsmentioning

confidence: 99%

Orbital, precessional and flaring variability of Cygnus X-1

Brocksopp¹,

Fender²,

Larionov³

et al. 1999

Monthly Notices of the Royal Astronomical Society

150

197

View full text Add to dashboard Cite

show abstract

“…We use this to deduce that Larwood's model fits our data if we assume i 208. This is rather low (e.g., Bruevich et al 1978 suggest i 408±608 and Kemp et al 1979 suggest i 608±708), and so it appears that some refinement to the model is necessary. The radiative warping model of Wijers & Pringle (1999) predicts a long-period of 180 d for Cyg X-1.…”

Section: The Long-term Periodmentioning

confidence: 98%

Orbital, Precessional and Flaring Variability in Cygnus X-1

Brocksopp¹,

Fender²,

Larianov³

et al.

Black Holes in Binaries and Galactic Nuclei: Diagnostics, Demography and Formation

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We present the results of a 2.5-year multiwavelength monitoring programme of Cygnus X-1, making use of hard and soft X-ray data, optical spectroscopy, UBVJHK photometry and radio data. In particular we confirm that the 5.6-day orbital period is apparent in all wavebands and note the existence of a wavelength-dependence to the modulation, in the sense that higher energies reach minimum first. We also find a strong modulation at a period of 142 ± 7 days, which we suggest is due to precession and/or radiative warping of the accretion disc. Strong modulation of the hard and soft X-ray flux at this long period may not be compatible with simple models of an optically thin accretion flow and corona in the low state. We present the basic components required for more detailed future modelling of the system -including a partially optically thick jet, quasi-continuous in the low state, the base of which acts as the Comptonising corona. In addition, we find that there are a number of flares which appear to be correlated in at least two wavebands and generally in more. We choose two of these flares to study in further detail and find that the hard and soft X-rays are well-correlated in the first and that the soft X-rays and radio are correlated in the second. In general, the optical and infrared show similar behaviour to each other but are not correlated with the X-rays or radio.

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“…S8-S9, and Table S4). The optical polarization directions is believed to give the orientation of the orbital axis onto the sky (27).…”

Section: Ixpementioning

confidence: 99%

“…We note that the blue supergiant HDE 226868 companion star dominates the optical emission (21). The optical polarization is likely produced by the scattering of the stellar radiation off the bulge formed by the accretion stream interacting with the accretion disk (27). The bottom panel shows residuals (contributions to χ).…”

Section: Optical Polarimetrymentioning

confidence: 99%

Polarized x-rays constrain the disk-jet geometry in the black hole x-ray binary Cygnus X-1

Krawczynski,

Muleri,

Dovčiak

et al. 2022

Preprint

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Cygnus X-1 - Polarization evidence for an extended secondary envelope with an eclipsing region

Cited by 19 publications

References 0 publications

Orbital, precessional and flaring variability of Cygnus X-1

Orbital, precessional and flaring variability of Cygnus X-1

Orbital, Precessional and Flaring Variability in Cygnus X-1

Polarized x-rays constrain the disk-jet geometry in the black hole x-ray binary Cygnus X-1

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