Testing reflection features in 4U 1705−44 with<i>XMM-Newton</i>,<i>BeppoSAX</i>, and RXTE in the hard and soft states

Egron, E.; Salvo, T. Di; Motta, S.; Burderi, L.; Papitto, A.; Duro, Refiz; D’Aí, A.; Riggio, A.; Belloni, T.; Iaria, R.; Robba, N. R.; Piraino, S.; Santangelo, A.

doi:10.1051/0004-6361/201219675

Cited by 56 publications

(89 citation statements)

References 63 publications

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“…Unfortunately, Model1 cannot be applied to the B1, B2, or B3 spectra because in the banana state the electron cloud temperature is ∼3 keV (Piraino et al 2007;Di Salvo et al 2009;Egron et al 2013), while the compPS component was considered for electron cloud temperatures T e > 10 keV. We also tried to fit the island state spectrum I using the alternative model wabs*(diskline+compTT+compPS) (Model2), containing a soft Comptonization component (compTT) with spherical geometry, plus a second hard Comptonization component (compPS) with disk geometry.…”

Section: Spectral Analysismentioning

confidence: 99%

“…The addition of a blackbody component to this model was not statistically significant, suggesting that we did not observe the seed photon component. Recently, Egron et al (2013), combining data from XMM-Newton, RXTE, and BeppoSAX (with the exclusion of the PDS instrument), obtained a similar spectral deconvolution using the model phabs*(nthComp+highecut*rdblur*reflionx), which contains a thermally Comptonized continuum (nthComp; Zdziarski et al 1996;Zycki et al 1999) plus a self-consistent reflection model including both the reflection continuum and the corresponding discrete features (Ross & Fabian 2005). The relativistically smeared rdblur kernel (Fabian et al 1989) was also used.…”

Section: The Island Statementioning

confidence: 99%

“…The broad line of 4U 1705-44, with others lines detected with XMM-Newton, is also discussed in Ng et al (2010) who point out the potential role of the pileup in the broadening of the line. However, recent developments of the subject can be found in Di Salvo et al (2015), Cackett & Miller (2013), Sanna et al (2013), Egron et al (2013), Piraino et al (2012), Cackett et al (2012), andMiller et al (2010).…”

Section: Introductionmentioning

confidence: 99%

“…The same data have already been partially used by Fiocchi et al (2007), Lin et al (2010), Cackett et al (2012), and Egron et al (2013). In fact, our analysis alone uses all BeppoSAX NFIs for both observations.…”

Section: Introductionmentioning

confidence: 99%

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Broadband observations of the X-ray burster 4U1705-44 withBeppoSAX

Piraino

Santangelo

Mück

et al. 2016

A&A

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Context. 4U 1705-44 is one of the most-studied type I X-ray burster and Atoll sources. This source represents a perfect candidate to test different models proposed to self-consistently track the physical changes occurring between different spectral states because it shows clear spectral state transitions. Aims. The broadband coverage, the sensitivity and energy resolution of the BeppoSAX satellite offers the opportunity to disentangle the components that form the total X-ray spectrum and to study their changes according to the spectral state. Methods. Using two BeppoSAX observations carried out in August and October 2000, respectively, for a total effective exposure time of ∼100 ks, we study the spectral evolution of the source from a soft to hard state. Energy spectra are selected according to the source position in the color-color diagram (CCD). Results. We succeeded in modeling the spectra of the source using a physical self-consistent scenario for both the island and banana branches (the double Comptonization scenario). The components observed are the soft Comptonization and hard Comptonization, the blackbody, and a reflection component with a broad iron line. When the source moves from the banana state to the island state, the parameters of the two Comptonization components change significantly and the blackbody component becomes too weak to be detected. Conclusions. We interpret the soft Comptonization component as emission from the hot plasma surrounding the neutron star, hard Comptonization as emission from the disk region, and the blackbody component as emission from the inner accretion disk. The broad feature in the iron line region is compatible with reflection from the inner accretion disk.

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Section: Spectral Analysismentioning

confidence: 99%

Section: The Island Statementioning

confidence: 99%

Section: Introductionmentioning

confidence: 99%

Section: Introductionmentioning

confidence: 99%

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Broadband observations of the X-ray burster 4U1705-44 withBeppoSAX

Piraino

Santangelo

Mück

et al. 2016

A&A

Self Cite

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“…Broad iron line profiles have been seen in these accreting systems that harbor a black hole (e.g., Fabian et al 1989;Miller 2007;Reis et al 2008Reis et al , 2009a or a neutron star (NS; e.g., Bhattacharyya & Strohmayer 2007;Cackett et al 2008Cackett et al , 2009Cackett et al , 2010Papitto et al 2008;di Salvo et al 2009;Egron et al 2013;Miller et al 2013) as the primary accreting compact object. The asymmetrically, broadened profile of the Fe a K line gives a direct measure of the position of the inner disk since the effects of gravitational redshift and Doppler redshift/boosting on the emission line become stronger closer to the compact object (Fabian et al 1989).…”

Section: Introductionmentioning

confidence: 99%

Nustar and XMM-Newton Observations of the Neutron Star X-Ray Binary 1rxs J180408.9-34205

Ludlam

Miller

Cackett

et al. 2016

ApJ

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We report on observations of the neutron star (NS) residing in the low-mass X-ray binary 1RXS J180408.9-34205 taken 2015 March by NuSTAR and XMM-Newton while the source was in the hard spectral state. We find multiple reflection features (Fe a K detected with NuSTAR; N VII, O VII, and O VIII detected in the RGS) from different ionization zones. Through joint fits using the self-consistent relativistic reflection model RELXILL, we determine the inner radius to be 11.1 R g . For a 1.4  M NS with a spin of * = a 0, this is an inner disk radius of 22.2 km. We find the inclination of the system to be between 18°and 29°. If the disk is truncated at a radius greater than the NS radius, it could be truncated by a boundary layer on the NS surface. It is also possible that the disk is truncated at the magnetospheric radius; conservative estimates would then imply ( -) B 0.3 1.0 10 9 G at the magnetic poles, though coherent pulsations have not been detected and the source is not identified as a pulsar.

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High-Frequency Variability in Neutron-Star Low-Mass X-ray Binaries

Méndez

Belloni

2020

Astrophysics and Space Science Library

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Binary systems with a neutron-star primary accreting from a companion star display variability in the X-ray band on time scales ranging from years to milliseconds. With frequencies of up to ∼1300 Hz, the kilohertz quasi-periodic oscillations (kHz QPOs) represent the fastest variability observed from any astronomical object. The sub-millisecond time scale of this variability implies that the kHz QPOs are produced in the accretion flow very close to the surface of the neutron star, providing a unique view of the dynamics of matter under the influence of some of the strongest gravitational fields in the Universe. This offers

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Testing reflection features in 4U 1705−44 withXMM-Newton,BeppoSAX, and RXTE in the hard and soft states

Cited by 56 publications

References 63 publications

Broadband observations of the X-ray burster 4U1705-44 withBeppoSAX

Broadband observations of the X-ray burster 4U1705-44 withBeppoSAX

Nustar and XMM-Newton Observations of the Neutron Star X-Ray Binary 1rxs J180408.9-34205

High-Frequency Variability in Neutron-Star Low-Mass X-ray Binaries

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