Secular spin-down of the AMP XTE J1751-305

Tiziana Di Salvo, Rosario Iaria, Burderi, Menna, Papitto, Riggio

Risultato della ricerca: Article

20 Citazioni (Scopus)

Abstract

Context. Of the 13 known accreting millisecond pulsars, only a few have displayed more than one outburst during the RXTEera. After its main outburst in 2002, XTE J1751-305 showed an additional three dim outbursts. We report on the timing analysis of the latest one, which occurred on October 8, 2009 and was serendipitously observed from its very beginning by RXTE. Aims: By detecting the pulsation during more than one outburst, we derive a stronger constraint of the orbital parameters and their evolution, and we can track the secular spin frequency evolution of the source. Methods: Using the RXTEdata of the last outburst of the AMP XTE J1751-305, we performed a timing analysis to more accurately constrain the orbital parameters. Because of the low quality of the data statistics, we applied an epoch-folding search technique to the whole data set to improve the local estimate of the time of ascending node passage. Results: Using this new orbital solution, we epoch-folded data obtaining three pulse phase delays over a time span of 1.2 days, that we fitted using a constant spin frequency model. Comparing this barycentric spin frequency with that of the 2002 outburst, we obtained a secular spin frequency derivative of -0.55(12) × 10-14 Hz s-1. We estimate the pulsar's magnetic dipole value by assuming that the secular spin-down is due to a rotating magneto dipole emission, to be consistent with what is assumed for radio pulsars. We derive an estimate of the magnetic field strength at the polar cap of BPC = 4.0(4) × 108 G, for a neutron star mass of 1.4 Msun, assuming the Friedman Pandharipande Skyrme equation of state.
Lingua originaleEnglish
pagine (da-a)-
Numero di pagine7
RivistaASTRONOMY & ASTROPHYSICS
Volume531
Stato di pubblicazionePublished - 2011

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adenosine monophosphate
outburst
time measurement
pulsars
orbitals
estimates
X Ray Timing Explorer
polar caps
magnetic dipoles
folding
neutron stars
field strength
equation of state
equations of state
statistics
dipoles
radio
magnetic field
pulses
magnetic fields

All Science Journal Classification (ASJC) codes

  • Astronomy and Astrophysics
  • Space and Planetary Science

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Secular spin-down of the AMP XTE J1751-305. / Di Salvo, Tiziana; Iaria, Rosario; Burderi; Menna; Papitto; Riggio.

In: ASTRONOMY & ASTROPHYSICS, Vol. 531, 2011, pag. -.

Risultato della ricerca: Article

Di Salvo, T, Iaria, R, Burderi, Menna, Papitto & Riggio 2011, 'Secular spin-down of the AMP XTE J1751-305', ASTRONOMY & ASTROPHYSICS, vol. 531, pagg. -.
Di Salvo, Tiziana ; Iaria, Rosario ; Burderi ; Menna ; Papitto ; Riggio. / Secular spin-down of the AMP XTE J1751-305. In: ASTRONOMY & ASTROPHYSICS. 2011 ; Vol. 531. pagg. -.
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abstract = "Context. Of the 13 known accreting millisecond pulsars, only a few have displayed more than one outburst during the RXTEera. After its main outburst in 2002, XTE J1751-305 showed an additional three dim outbursts. We report on the timing analysis of the latest one, which occurred on October 8, 2009 and was serendipitously observed from its very beginning by RXTE. Aims: By detecting the pulsation during more than one outburst, we derive a stronger constraint of the orbital parameters and their evolution, and we can track the secular spin frequency evolution of the source. Methods: Using the RXTEdata of the last outburst of the AMP XTE J1751-305, we performed a timing analysis to more accurately constrain the orbital parameters. Because of the low quality of the data statistics, we applied an epoch-folding search technique to the whole data set to improve the local estimate of the time of ascending node passage. Results: Using this new orbital solution, we epoch-folded data obtaining three pulse phase delays over a time span of 1.2 days, that we fitted using a constant spin frequency model. Comparing this barycentric spin frequency with that of the 2002 outburst, we obtained a secular spin frequency derivative of -0.55(12) × 10-14 Hz s-1. We estimate the pulsar's magnetic dipole value by assuming that the secular spin-down is due to a rotating magneto dipole emission, to be consistent with what is assumed for radio pulsars. We derive an estimate of the magnetic field strength at the polar cap of BPC = 4.0(4) × 108 G, for a neutron star mass of 1.4 Msun, assuming the Friedman Pandharipande Skyrme equation of state.",
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T1 - Secular spin-down of the AMP XTE J1751-305

AU - Di Salvo, Tiziana

AU - Iaria, Rosario

AU - Burderi, null

AU - Menna, null

AU - Papitto, null

AU - Riggio, null

PY - 2011

Y1 - 2011

N2 - Context. Of the 13 known accreting millisecond pulsars, only a few have displayed more than one outburst during the RXTEera. After its main outburst in 2002, XTE J1751-305 showed an additional three dim outbursts. We report on the timing analysis of the latest one, which occurred on October 8, 2009 and was serendipitously observed from its very beginning by RXTE. Aims: By detecting the pulsation during more than one outburst, we derive a stronger constraint of the orbital parameters and their evolution, and we can track the secular spin frequency evolution of the source. Methods: Using the RXTEdata of the last outburst of the AMP XTE J1751-305, we performed a timing analysis to more accurately constrain the orbital parameters. Because of the low quality of the data statistics, we applied an epoch-folding search technique to the whole data set to improve the local estimate of the time of ascending node passage. Results: Using this new orbital solution, we epoch-folded data obtaining three pulse phase delays over a time span of 1.2 days, that we fitted using a constant spin frequency model. Comparing this barycentric spin frequency with that of the 2002 outburst, we obtained a secular spin frequency derivative of -0.55(12) × 10-14 Hz s-1. We estimate the pulsar's magnetic dipole value by assuming that the secular spin-down is due to a rotating magneto dipole emission, to be consistent with what is assumed for radio pulsars. We derive an estimate of the magnetic field strength at the polar cap of BPC = 4.0(4) × 108 G, for a neutron star mass of 1.4 Msun, assuming the Friedman Pandharipande Skyrme equation of state.

AB - Context. Of the 13 known accreting millisecond pulsars, only a few have displayed more than one outburst during the RXTEera. After its main outburst in 2002, XTE J1751-305 showed an additional three dim outbursts. We report on the timing analysis of the latest one, which occurred on October 8, 2009 and was serendipitously observed from its very beginning by RXTE. Aims: By detecting the pulsation during more than one outburst, we derive a stronger constraint of the orbital parameters and their evolution, and we can track the secular spin frequency evolution of the source. Methods: Using the RXTEdata of the last outburst of the AMP XTE J1751-305, we performed a timing analysis to more accurately constrain the orbital parameters. Because of the low quality of the data statistics, we applied an epoch-folding search technique to the whole data set to improve the local estimate of the time of ascending node passage. Results: Using this new orbital solution, we epoch-folded data obtaining three pulse phase delays over a time span of 1.2 days, that we fitted using a constant spin frequency model. Comparing this barycentric spin frequency with that of the 2002 outburst, we obtained a secular spin frequency derivative of -0.55(12) × 10-14 Hz s-1. We estimate the pulsar's magnetic dipole value by assuming that the secular spin-down is due to a rotating magneto dipole emission, to be consistent with what is assumed for radio pulsars. We derive an estimate of the magnetic field strength at the polar cap of BPC = 4.0(4) × 108 G, for a neutron star mass of 1.4 Msun, assuming the Friedman Pandharipande Skyrme equation of state.

KW - stars: neutron, stars: magnetic field, pulsars: general, pulsars: individual:XTE J1751-305, X-rays: binaries

UR - http://hdl.handle.net/10447/61917

UR - http://adsabs.harvard.edu/abs/2011A%26A...531A.140R

M3 - Article

VL - 531

SP - -

JO - Astronomy and Astrophysics

JF - Astronomy and Astrophysics

SN - 0004-6361

ER -