Search results for "X-ray: general"

showing 3 items of 3 documents

Spectral Evolution of Scorpio X‐1 along its Color‐Color Diagram

2007

We analyze a large collection of RXTE archive data of the bright X‐ray source Scorpius X‐1 in order to study the broadband spectral evolution of the source for different values of the inferred mass accretion rate by selecting energy spectra from its Color‐Color Diagram. We model the spectra with the combination of two absorbed components: a soft thermal component, which can be interpreted as thermal emission from an accretion disk, and a hybrid Comptonization component, which self‐consistently includes the Fe Kα fluorescence line and the Compton reflected continuum. The presence of hard emission in Scorpius X‐1 has been previously reported, however, without a clear relation with the accreti…

PhysicsAccretion (meteorology)Astrophysics::High Energy Astrophysical PhenomenaContinuum (design consultancy)X-ray: generalCompton scatteringX-ray binaryColor–color diagramAstrophysicsindividual: Scorpio X-1; Stars: neutron stars; X-ray: general; X-ray: spectrum; X-ray: stars [Accretion discs; Stars]X-ray: spectrumAstronomical spectroscopySpectral lineStars: neutron starX-ray: starsAccretion discStars: individual: Scorpio X-1Astrophysics::Galaxy AstrophysicsLine (formation)AIP Conference Proceedings
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A self-consistent approach to the reflection component in 4U 1705-44

2010

High-resolution spectroscopy has recently revealed in many neutron-star Low-Mass X-ray binaries that the shape of the broad iron line observed in the 6.4-6.97 keV range is consistently well fitted by a relativistically smeared line profile. We show here spectral fitting results using a newly developed self-consistent reflection model on XMM-Newton data of the LMXB 4U 1705-44 during a period when the source was in a bright soft state. This reflection model adopts a blackbody prescription for the shape of the impinging radiation field, that we physically associate with the boundary layer emission. © 2010 American Institute of Physics.

Physicsindividual: 4U 1705-44; stars: neutron stars; X-ray: general; X-ray: spectrum; X-ray: stars; Physics and Astronomy (all) [accretion discs; stars]stars: neutron starAstrophysics::High Energy Astrophysical PhenomenaX-ray: generalX-ray binaryCosmic background radiationX-ray: starAstrophysicsX-ray: spectrumstars: individual: 4U 1705-44Interstellar mediumPhysics and Astronomy (all)accretion discReflection (physics)Black-body radiationInfrared cirrusSpectroscopyLine (formation)
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A method to constrain the neutron star magnetic field in Low Mass X-ray Binaries

2005

We describe here a method to put an upper limit to the strength of the magnetic field of neutron stars in low mass X‐ray binaries for which the spin period and the X‐ray luminosity during X‐ray quiescent periods are known. This is obtained using simple considerations about the position of the magnetospheric radius during quiescent periods. We applied this method to the accreting millisecond pulsar SAX J1808.4‐3658, which shows coherent X‐ray pulsations at a frequency of ∼ 400 Hz and a quiescent X‐ray luminosity of ∼ 5 × 1031 ergs/s, and found that B ⩽ 5 × 108 Gauss in this source. Combined with the lower limit inferred from the presence of X‐ray pulsations, this constrains the SAX J1808.4‐3…

PhysicsX-ray: binarieAstrophysics::High Energy Astrophysical PhenomenaStars: individual: SAX J1808.4-3658 KS 1731-260 Aql X-1X-ray: generalX-ray binaryAstronomyAstrophysics::Cosmology and Extragalactic AstrophysicsAstrophysicsRadiusindividual: SAX J1808.4-3658 KS 1731-260 Aql X-1; Stars: neutron stars; X-ray: binaries; X-ray: general; X-ray: stars [Accretion discs; Stars]LuminosityMagnetic fieldStars: neutron starNeutron starPulsarMillisecond pulsarAstrophysics::Solar and Stellar AstrophysicsX-ray: starsAccretion discLow MassAstrophysics::Galaxy Astrophysics
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