Hume's Philosophical Politics. By Duncan Forbes. Cambridge University Press. 1975. Pp. 338. £9.90.

Whelan, Frederick G.

doi:10.1017/s0018246x00011055

Cited by 10 publications

(14 citation statements)

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“…Based on the properties of the type I X-ray bursts, Jonker & Nelemans (2004) estimated a distance to the source of 7.8-10.5 kpc; according to a different measure of the Galactic absorption, Iaria et al (2005) derived a lower distance of 4.1 kpc (but see Jonker, Nelemans & Bassa 2007). E-mail: p.soleri@uva.nl Cir X−1 is the most radio-loud neutron star X-ray binary (Whelan et al 1977;Haynes et al 1978; Cyg X−3 and SS433 are brighter in radio but their nature is unclear) showing extended structures both at arcmin and arcsec scale. The arcmin-scale structure has been extensively studied by Stewart et al (1993) and Tudose et al (2006): the source shows two radio jets (south-east and north-west direction) embedded in a large scale, diffuse radio nebula.…”

Section: Introductionmentioning

confidence: 99%

A parsec scale X-ray extended structure from the X-ray binary Circinus X–1

Soleri

Heinz

Fender

et al. 2009

Monthly Notices of the Royal Astronomical Society: Letters

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We present the results of the analysis of two Chandra observations of Circinus X−1 performed in 2007, for a total exposure time of ∼50 ks. The source was observed with the High Resolution Camera during a long X‐ray low‐flux state of the source. Cir X−1 is an accreting neutron star binary system that exhibits ultra‐relativistic arcsec‐scale radio jets and an extended arcmin‐scale radio nebula. Furthermore, a recent paper has shown an X‐ray excess on arcmin‐scale prominent on the side of the receding radio jet. In our images, we clearly detect X‐ray structures on both the side of the receding and the approaching radio jet. The X‐ray emission is consistent with a synchrotron origin. Our detection is consistent with neutron star binaries being as efficient as black hole binaries in producing X‐ray outflows, despite their shallower gravitational potential.

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Section: Introductionmentioning

confidence: 99%

A parsec scale X-ray extended structure from the X-ray binary Circinus X–1

Soleri

Heinz

Fender

et al. 2009

Monthly Notices of the Royal Astronomical Society: Letters

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“…However, the compact object is also believed to be a neutron star because of the presence of type I X-ray bursts ( Tennant et al 1986a( Tennant et al , 1986b. The radio counterpart of Cir X-1, coincident with a faint red star, displays flares with the same periodicity as the orbital period (Whelan et al 1977), and its IR characteristics also show periodicity (Glass 1978). Its optical counterpart has been proven to be a faint red star ( Moneti 1992).…”

Section: Introductionmentioning

confidence: 99%

Evolution of Hard X‐Ray Spectra along the Orbital Phase in Circinus X‐1

Ding

Zhang

et al. 2006

ApJ

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Using the data from the Proportional Counter Array and the High-Energy X-Ray Timing Experiment on board the Rossi X-Ray Timing Explorer satellite, we investigate the evolution of the 3-200 keV spectrum of the peculiar lowmass X-ray binary Circinus X-1 along its orbital phase. A power-law hard component, dominating above $30 keVas well as contributing between 0.9% and 3.5% of the total flux, and the iron emission line are detected in the spectrum. It is found that the derived photon index (À) of the power-law hard component and the characteristics of the iron emission line are modulated by the orbital phase: the hardest hard tail, the lowest line energy, and the largest line width of the iron emission line are detected at the periastron. However, the softest hard tail, the highest line energy, and the lowest line width of the iron emission line are detected after the apastron. At the periastron the source evolves along a complete track in the color-color diagram. These behaviors of orbital modulation are discussed. A possible origin of the power-law hard component is also discussed.

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“…However, the compact object is also believed to be a neutron star (NS) because of the presence of type I X-ray bursts (Tennant, Fabian, & Shafer 1986a, 1986b. The radio counterpart of Cir X-1, coincident with a faint red star, displays flares with the same periodicity as the orbital period (Whelan et al 1977); its IR characteristics also show periodicity (Glass 1978); and its optical counterpart has proved to be a faint red star (Moneti 1992). The soft Xray (3-6 keV) flux of Cir X-1 shows a well-defined periodic modulation with the same period as its orbital period (Kaluzienski et al 1976).…”

Section: Introductionmentioning

confidence: 99%

Evolution of Hard X-Ray Spectra along the Branches in Circinus X-1

Ding

2003

ApJ

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Using the data from the Proportional Counter Array and the High-Energy X-Ray Timing Experiment on board the Rossi X-Ray Timing Explorer satellite, we investigate the evolution of the 3-200 keV spectra of the peculiar low-mass X-ray binary Circinus X-1 along the branches on its hardness-intensity diagram (HID) from the vertical horizontal branch, through the horizontal horizontal branch and normal branch, to the flaring branch. We detect a power-law hard component in the spectra. It is found that the derived photon indices (G) of the power-law hard component are correlated with the position on the HID. The power-law component dominates the X-ray emission of Cir X-1 in the energy band higher than ∼20 keV. The fluxes of the power-law component are compared with those of the bremsstrahlung component in the spectra. A possible origin of the power-law hard component is discussed.

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Hume's Philosophical Politics. By Duncan Forbes. Cambridge University Press. 1975. Pp. 338. £9.90.

Cited by 10 publications

References 0 publications

A parsec scale X-ray extended structure from the X-ray binary Circinus X–1

A parsec scale X-ray extended structure from the X-ray binary Circinus X–1

Evolution of Hard X‐Ray Spectra along the Orbital Phase in Circinus X‐1

Evolution of Hard X-Ray Spectra along the Branches in Circinus X-1

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