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

Rosario Iaria, Angelo Francesco Gambino, Tiziana Di Salvo, D'Aì, Esposito, Riggio, Bozzo, Pintore, Sanna, Segreto, Scarano, Burderi

Risultato della ricerca: Article

4 Citazioni (Scopus)

Abstract

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 as nu proportional to M-beta, we fitted the pulse phase delays obtaining a value of beta = 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 and 4.1 kpc, assuming a disc viscous parameter a to be in the range of 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.
Lingua originaleEnglish
pagine (da-a)2-12
Numero di pagine11
RivistaMonthly Notices of the Royal Astronomical Society
Volume469
Stato di pubblicazionePublished - 2017

Fingerprint

torque
outburst
pulsars
accretion
x rays
pulses
time measurement
XMM-Newton telescope
newton
spectrum analysis
analysis
rate

All Science Journal Classification (ASJC) codes

  • Astronomy and Astrophysics
  • Space and Planetary Science

Cita questo

Study of the accretion torque during the 2014 outburst of the X-ray pulsar GRO J1744−28. / Iaria, Rosario; Gambino, Angelo Francesco; Di Salvo, Tiziana; D'Aì; Esposito; Riggio; Bozzo; Pintore; Sanna; Segreto; Scarano; Burderi.

In: Monthly Notices of the Royal Astronomical Society, Vol. 469, 2017, pag. 2-12.

Risultato della ricerca: Article

@article{3ca1a1d0d0af49e7ab98a95f815e30f7,
title = "Study of the accretion torque during the 2014 outburst of the X-ray pulsar GRO J1744−28",
abstract = "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 as nu proportional to M-beta, we fitted the pulse phase delays obtaining a value of beta = 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 and 4.1 kpc, assuming a disc viscous parameter a to be in the range of 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.",
author = "Rosario Iaria and Gambino, {Angelo Francesco} and {Di Salvo}, Tiziana and D'A{\`i} and Esposito and Riggio and Bozzo and Pintore and Sanna and Segreto and Scarano and Burderi",
year = "2017",
language = "English",
volume = "469",
pages = "2--12",
journal = "Monthly Notices of the Royal Astronomical Society",
issn = "0035-8711",
publisher = "Oxford University Press",

}

TY - JOUR

T1 - Study of the accretion torque during the 2014 outburst of the X-ray pulsar GRO J1744−28

AU - Iaria, Rosario

AU - Gambino, Angelo Francesco

AU - Di Salvo, Tiziana

AU - D'Aì, null

AU - Esposito, null

AU - Riggio, null

AU - Bozzo, null

AU - Pintore, null

AU - Sanna, null

AU - Segreto, null

AU - Scarano, null

AU - Burderi, null

PY - 2017

Y1 - 2017

N2 - 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 as nu proportional to M-beta, we fitted the pulse phase delays obtaining a value of beta = 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 and 4.1 kpc, assuming a disc viscous parameter a to be in the range of 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.

AB - 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 as nu proportional to M-beta, we fitted the pulse phase delays obtaining a value of beta = 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 and 4.1 kpc, assuming a disc viscous parameter a to be in the range of 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.

UR - http://hdl.handle.net/10447/249428

M3 - Article

VL - 469

SP - 2

EP - 12

JO - Monthly Notices of the Royal Astronomical Society

JF - Monthly Notices of the Royal Astronomical Society

SN - 0035-8711

ER -