Broad Relativistic Iron Emission Line Observed in Sax J1808.4–3658

Cackett, Edward M.; Altamirano, D.; Patruno, A.; Miller, J. M.; Reynolds, M. T.; Linares, M.; Wijnands, Rudy

doi:10.1088/0004-637x/694/1/l21

Cited by 122 publications

(181 citation statements)

References 33 publications

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“…However, other studies find lower ionization parameter values for an NS in the LHS (Cackett et al 2009;Papitto et al 2009;D'Aì et al 2010;Di Salvo et al 2015). However, it is likely that some of the emergent flux in the iron line region for 1RXS J1804 is partially from a region of lower ionization.…”

Section: Discussionmentioning

confidence: 85%

“…We can place an upper limit on the strength of the field using the upper limit of = R 1.85 in ISCO. Assuming a mass of 1.4  M , taking the distance to be 5.8 kpc (Krimm et al 2015b), and using the unabsorbed flux from 0.45 to 50.0 keV of -1.71 10 9 erg cm −2 s −1 as the bolometric flux, we can determine the magnetic dipole moment, μ, from Equation (1) taken from Cackett et al (2009): If we make the same assumptions about geometry and accretion efficiency (i.e.,…”

Section: Nustar+rgsmentioning

confidence: 99%

“…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%

“…Constraining the radius of the NS can, in turn, lead to narrowing down the equation of state of the cold, dense matter under extremely dense physical conditions (Lattimer 2011). On the other hand, if the accretion rate is low, it may be possible to constrain the stellar magnetic field based on the radius at which the disk truncates (Cackett et al 2009;Papitto et al 2009;Miller et al 2011;Degenaar et al 2014).…”

Section: Introductionmentioning

confidence: 99%

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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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Section: Discussionmentioning

confidence: 85%

Section: Nustar+rgsmentioning

confidence: 99%

Section: Introductionmentioning

confidence: 99%

Section: Introductionmentioning

confidence: 99%

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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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“…Even in the case of accreting millisecond pulsars (AMSPs), which are usually found in a hard state and for which we expect that the inner disk is truncated by the magnetic field, inner disk radii in the range 6 − 40 R g were usually found (see, e.g. Papitto et al 2009;Cackett et al 2009;Papitto et al 2010Papitto et al , 2013aKing et al 2016). Also, the reflection fraction inferred from the rfxconv model, Ω/2π ∼ 0.22, although somewhat smaller than what is expected for a geometry with a spherical corona surrounded by the accretion disk (Ω/2π ∼ 0.3), is in agreement with typical values for these sources.…”

Section: The Combined Xmm-newton and Integral Spectrummentioning

confidence: 99%

XMM-Newtonand INTEGRAL view of the hard state of EXO 1745−248 during its 2015 outburst

Matranga

Papitto

Salvo

et al. 2017

A&A

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Context. Transient low-mass X-ray binaries (LMXBs) often show outbursts lasting typically a few-weeks and characterized by a high X-ray luminosity (L x ≈ 10 36 − 10 38 erg s −1 ), while for most of the time they are found in X-ray quiescence (L X ≈ 10 31 − 10 33 erg s −1 ). EXO 1745-248 is one of them. Aims. The broad-band coverage, and the sensitivity of instrumet on board of XMM-Newton and INTEGRAL, offers the opportunity to characterize the hard X-ray spectrum during EXO 1745-248 outburst. Methods. In this paper we report on quasi-simultaneous XMM-Newton and INTEGRAL observations of the X-ray transient EXO 1745-248 located in the globular cluster Terzan 5, performed ten days after the beginning of the outburst (on 2015 March 16th) shown by the source between March and June 2015. The source was caught in a hard state, emitting a 0.8-100 keV luminosity of ≃ 10 37 erg s −1 . Results. The spectral continuum was dominated by thermal Comptonization of seed photons with temperature kT in ≃ 1.3 keV, by a cloud with moderate optical depth τ ≃ 2 and electron temperature kT e ≃ 40 keV. A weaker soft thermal component at temperature kT th ≃ 0.6-0.7 keV and compatible with a fraction of the neutron star radius was also detected. A rich emission line spectrum was observed by the EPIC-pn on-board XMM-Newton; features at energies compatible with K-α transitions of ionized sulfur, argon, calcium and iron were detected, with a broadness compatible with either thermal Compton broadening or Doppler broadening in the inner parts of an accretion disk truncated at 20 ± 6 gravitational radii from the neutron star. Strikingly, at least one narrow emission line ascribed to neutral or mildly ionized iron is needed to model the prominent emission complex detected between 5.5 and 7.5 keV. The different ionization state and broadness suggest an origin in a region located farther from the neutron star than where the other emission lines are produced. Seven consecutive type-I bursts were detected during the XMM-Newton observation, none of which showed hints of photospheric radius expansion. A thorough search for coherent pulsations from the EPIC-pn light curve did not result in any significant detection. Upper limits ranging from a few to 15% on the signal amplitude were set, depending on the unknown spin and orbital parameters of the system.

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Accretion Powered X-ray Millisecond Pulsars

Salvo

Sanna

2021

Astrophysics and Space Science Library

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Broad Relativistic Iron Emission Line Observed in Sax J1808.4–3658

Cited by 122 publications

References 33 publications

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

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

XMM-Newtonand INTEGRAL view of the hard state of EXO 1745−248 during its 2015 outburst

Accretion Powered X-ray Millisecond Pulsars

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