Physics of accretion in the millisecond pulsar XTE J1751 - 305

Marek Gierliński (Lead / Corresponding author), Juri Poutanen (Lead / Corresponding author)

Research output: Contribution to journalArticle

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Abstract

We have undertaken an extensive study of X-ray data from the accreting millisecond pulsar XTE J1751 - 305 observed by RXTE and XMM - Newton during its 2002 outburst. In all aspects this source is similar to the prototypical millisecond pulsar SAX J 1808.4 -3658, except for the higher peak luminosity of 13 per cent of Eddington, and the optical depth of the hard X-ray source, which is larger by a factor ∼2. Its broad-band X-ray spectrum can be modelled by three components. We interpret the two soft components as thermal emission from a colder (kT ∼0.6 keV) accretion disc and a hotter (∼1 keV) spot on the neutron star surface. We interpret the hard component as thermal Comptonization in plasma of temperature ∼40 keV and optical depth ∼ 1.5 in a slab geometry. The plasma is heated by the accretion shock as the material collimated by the magnetic field impacts on to the surface. The seed photons for Comptonization are provided by the hotspot, not by the disc. The Compton reflection is weak and the disc is probably truncated into an optically thin flow above the magnetospheric radius. Rotation of the emission region with the star creates an almost sinusoidal pulse profile with an rms amplitude of 3.3 per cent. The energy-dependent soft phase lags can be modelled by two pulsating components shifted in phase, which is naturally explained by a different character of emission of the optically thick spot and optically thin shock combined with the action of the Doppler boosting. The observed variability amplitude constrains the hotspot to lie within 3°-4° of the rotational pole. We estimate the inner radius of the optically thick accreting disc to be about 40 km. In that case, the absence of emission from the antipodal spot, which can be blocked by the accretion disc, gives the inclination of the system as ≳70°.

Original languageEnglish
Pages (from-to)1261-1276
Number of pages16
JournalMonthly Notices of the Royal Astronomical Society
Volume359
Issue number4
DOIs
Publication statusPublished - 1 Jun 2005

Fingerprint

pulsars
physics
accretion
accretion disks
optical thickness
optical depth
hot spot
shock
plasma
x rays
radii
X Ray Timing Explorer
thermal emission
XMM-Newton telescope
outburst
newton
neutron stars
inclination
seeds
slab

Keywords

  • Accretion, accretion discs
  • Pulsars: individual: XTE J1751 - 305
  • X-rays: binaries

Cite this

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title = "Physics of accretion in the millisecond pulsar XTE J1751 - 305",
abstract = "We have undertaken an extensive study of X-ray data from the accreting millisecond pulsar XTE J1751 - 305 observed by RXTE and XMM - Newton during its 2002 outburst. In all aspects this source is similar to the prototypical millisecond pulsar SAX J 1808.4 -3658, except for the higher peak luminosity of 13 per cent of Eddington, and the optical depth of the hard X-ray source, which is larger by a factor ∼2. Its broad-band X-ray spectrum can be modelled by three components. We interpret the two soft components as thermal emission from a colder (kT ∼0.6 keV) accretion disc and a hotter (∼1 keV) spot on the neutron star surface. We interpret the hard component as thermal Comptonization in plasma of temperature ∼40 keV and optical depth ∼ 1.5 in a slab geometry. The plasma is heated by the accretion shock as the material collimated by the magnetic field impacts on to the surface. The seed photons for Comptonization are provided by the hotspot, not by the disc. The Compton reflection is weak and the disc is probably truncated into an optically thin flow above the magnetospheric radius. Rotation of the emission region with the star creates an almost sinusoidal pulse profile with an rms amplitude of 3.3 per cent. The energy-dependent soft phase lags can be modelled by two pulsating components shifted in phase, which is naturally explained by a different character of emission of the optically thick spot and optically thin shock combined with the action of the Doppler boosting. The observed variability amplitude constrains the hotspot to lie within 3°-4° of the rotational pole. We estimate the inner radius of the optically thick accreting disc to be about 40 km. In that case, the absence of emission from the antipodal spot, which can be blocked by the accretion disc, gives the inclination of the system as ≳70°.",
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Physics of accretion in the millisecond pulsar XTE J1751 - 305. / Gierliński, Marek (Lead / Corresponding author); Poutanen, Juri (Lead / Corresponding author).

In: Monthly Notices of the Royal Astronomical Society, Vol. 359, No. 4, 01.06.2005, p. 1261-1276.

Research output: Contribution to journalArticle

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AU - Gierliński, Marek

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AB - We have undertaken an extensive study of X-ray data from the accreting millisecond pulsar XTE J1751 - 305 observed by RXTE and XMM - Newton during its 2002 outburst. In all aspects this source is similar to the prototypical millisecond pulsar SAX J 1808.4 -3658, except for the higher peak luminosity of 13 per cent of Eddington, and the optical depth of the hard X-ray source, which is larger by a factor ∼2. Its broad-band X-ray spectrum can be modelled by three components. We interpret the two soft components as thermal emission from a colder (kT ∼0.6 keV) accretion disc and a hotter (∼1 keV) spot on the neutron star surface. We interpret the hard component as thermal Comptonization in plasma of temperature ∼40 keV and optical depth ∼ 1.5 in a slab geometry. The plasma is heated by the accretion shock as the material collimated by the magnetic field impacts on to the surface. The seed photons for Comptonization are provided by the hotspot, not by the disc. The Compton reflection is weak and the disc is probably truncated into an optically thin flow above the magnetospheric radius. Rotation of the emission region with the star creates an almost sinusoidal pulse profile with an rms amplitude of 3.3 per cent. The energy-dependent soft phase lags can be modelled by two pulsating components shifted in phase, which is naturally explained by a different character of emission of the optically thick spot and optically thin shock combined with the action of the Doppler boosting. The observed variability amplitude constrains the hotspot to lie within 3°-4° of the rotational pole. We estimate the inner radius of the optically thick accreting disc to be about 40 km. In that case, the absence of emission from the antipodal spot, which can be blocked by the accretion disc, gives the inclination of the system as ≳70°.

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KW - X-rays: binaries

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