The Main Characteristics of GRO J1744−28 Observed by the Proportional Counter Array Experiment on the [ITAL]Rossi X-Ray Timing Explorer[/ITAL]

Giles, A. B.; Swank, J. H.; Jahoda, K.; Zhang, W.; Strohmayer, Tod E.; Stark, M. J.; Morgan, E.

doi:10.1086/310262

Cited by 75 publications

(71 citation statements)

References 19 publications

(18 reference statements)

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“…Such behaviour and the burst characteristics are very close to the typical phenomenology shown by the source in the two past outbursts (Giles et al 1996).…”

Section: Observation and Data Reductionsupporting

confidence: 78%

“…We observed to date three major X-ray outbursts from GRO J1744-28: the first associated with its discovery lasting from December 1995 to May 1996, where at the peak outburst reached over-Eddington luminosities (Jahoda et al 1999;Giles et al 1996;Woods et al 1999Woods et al , 2000; the second outburst occurred about one year later, started at the beginning of December 1996 and lasted about four months. A long period of quiescence followed, interrupted by the third and most recent outburst observed in January 2014.…”

Section: Introductionmentioning

confidence: 99%

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GRO J1744−28: an intermediate B-field pulsar in a low-mass X-ray binary

D’Aí

Salvo

Iaria

et al. 2015

Monthly Notices of the Royal Astronomical Society

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The bursting pulsar, GRO J1744-28, went again in outburst after ∼18 years of quiescence in mid-January 2014. We studied the broad-band, persistent, X-ray spectrum using X-ray data from a XMM-Newton observation, performed almost at the peak of the outburst, and from a close INTEGRAL observation, performed 3 days later, thus covering the 1.3-70.0 keV band. The spectrum shows a complex continuum shape that cannot be modelled with standard high-mass X-ray pulsar models, nor by twocomponents models. We observe broadband and peaked residuals from 4 to 15 keV, and we propose a self-consistent interpretation of these residuals, assuming they are produced by cyclotron absorption features and by a moderately smeared, highly ionized, reflection component. We identify the cyclotron fundamental at ∼ 4.7 keV, with hints for two possible harmonics at ∼ 10.4 keV and ∼ 15.8 keV. The position of the cyclotron fundamental allows an estimate for the pulsar magnetic field of (5.27 ± 0.06) × 10 11 G, if the feature is produced at its surface. From the dynamical and relativistic smearing of the disk reflected component, we obtain a lower limit estimate for the truncated accretion disk inner radius, ( 100 R g ), and for the inclination angle (18• -48 • ). We also detect the presence of a softer thermal component, that we associate with the emission from an accretion disk truncated at a distance from the pulsar of 50-115 R g . From these estimates, we derive the magneto-spheric radius for disk accretion to be ∼ 0.2 times the classical Alfvén radius for radial accretion.

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“…Such behaviour and the burst characteristics are very close to the typical phenomenology shown by the source in the two past outbursts (Giles et al 1996).…”

Section: Observation and Data Reductionsupporting

confidence: 78%

Section: Introductionmentioning

confidence: 99%

GRO J1744−28: an intermediate B-field pulsar in a low-mass X-ray binary

D’Aí

Salvo

Iaria

et al. 2015

Monthly Notices of the Royal Astronomical Society

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“…Based on the high values of the equivalent hydrogen column NH ∼ (0.5 − 1) × 10 23 atoms cm −2 , several authors placed an upper limit on the source distance in the range 7.5-8.5 kpc in correspondence with the Galactic center (e.g., Giles et al 1996;Augusteijn et al 1997;Nishiuchi et al 1999). On the other hand, a lower limit of 1.5 kpc and 2 kpc have been set from the analysis of the optical and near-infrared possible counterparts of the source, respectively (e.g., Cole et al 1997).…”

Section: Discussionmentioning

confidence: 99%

Study of the accretion torque during the 2014 outburst of the X-ray pulsar GRO J1744−28

Sanna

Riggio

Burderi

et al. 2017

Monthly Notices of the Royal Astronomical Society

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We present the spectral and timing analysis of the X-ray pulsar GRO J1744−28 during its 2014 outburst using data collected with the X-ray satellites Swift, INTEGRAL, Chandra, and XMM-Newton. We derived, by phase-connected timing analysis of the observed pulses, an updated set of the source ephemeris. We were also able to investigate the spin-up of the X-ray pulsar as a consequence of the accretion torque during the outburst. Relating the spin-up rate and the mass accretion rate asν ∝Ṁ β , we fitted the pulse phase delays obtaining a value of β = 0.96(3). Combining the results from the source spin-up frequency derivative and the flux estimation, we constrained the source distance to be between 3.4-4.1 kpc, assuming a disc viscous parameter α to be in the range 0.1-1. Finally, we investigated the presence of a possible spin-down torque by adding a quadratic component to the pulse phase delay model. The marginal statistical improvement of the updated model does not allow us to firmly confirm the presence of this component.

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“…Thus we conclude that the partial covering model is not preferred over the disk line model. Giles et al (1996) with the RXT E PCA data ; their analysis, however, was preliminary. The stable implies that the column density can be attributed to the N H interstellar absorption.…”

Section: Iron Featurementioning

confidence: 99%

ASCAObservations of GRO J1744−28

Nishiuchi

Koyama

Maeda

et al. 1999

ApJ

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We report the ASCA results of the bursting X-ray pulsar GRO J1744[28, which was observed in 1996 February and 1997 March. The source Ñux in the 2È10 keV band was 2.0 ] 10~8 ergs s~1 cm2 in 1996 and 5.0 ] 10~9 ergs s~1 cm2 in 1997. We detected 12 and 17 type II bursts during the two observations, with mean bursting intervals of about 27 min and 37 min. Each burst is followed by an intensity dip with the depleted Ñux depending on the burst Ñuence. The energy spectra are approximated by an absorbed power law with additional structure around 6È7 keV. The constant absorption column, (5È 6) ] 1022 cm~2, independent of the observation dates and emission phases (persistent, burst, and dip) is interpreted as an interstellar absorption. The source may be actually located near the Galactic center, at a distance of 8.5 kpc. The structure in the energy spectrum at 6È7 keV is most probably due to iron and may be reproduced by a disk line model with additional broadening mechanism.

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The Main Characteristics of GRO J1744−28 Observed by the Proportional Counter Array Experiment on the [ITAL]Rossi X-Ray Timing Explorer[/ITAL]

Cited by 75 publications

References 19 publications

GRO J1744−28: an intermediate B-field pulsar in a low-mass X-ray binary

GRO J1744−28: an intermediate B-field pulsar in a low-mass X-ray binary

Study of the accretion torque during the 2014 outburst of the X-ray pulsar GRO J1744−28

ASCAObservations of GRO J1744−28

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