Timing of the 2008 outburst of SAX J1808.4–3658   with XMM-Newton:
a stable orbital-period derivative over ten years

Burderi, L.; Riggio, A.; Salvo, T. Di; Papitto, A.; Menna, M. T.; D’Aí, A.; Iaria, R.

doi:10.1051/0004-6361/200811542

Cited by 58 publications

(107 citation statements)

References 20 publications

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“…In particular, the power injected by the pulsar into the companion of SAX J1808.4-3658 has been suggested to generate a large mass-loss (di Salvo et al 2008;Burderi et al 2009) which in turn would explain the large orbitalṖ b . In this highly non conservative mass-transfer scenario about 99% of the mass transferred is lost in a stellar wind.…”

Section: Resultsmentioning

confidence: 99%

“…The irradiation of the donor from a pulsar wind is a particularly interesting feature because it has been suggested as the mechanism at the origin of the peculiar orbital evolution of SAX J1808. 4-3658 (di Salvo et al 2008;Burderi et al 2009) which is expanding on a very short timescale of ∼ 70 Myr instead of the expected billion years predicted by the theory of angular momentum loss from gravitational waves (Hartman et al 2008;.…”

Section: Introductionmentioning

confidence: 99%

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The Slow Orbital Evolution of the Accreting Millisecond Pulsar IGR J0029+5934

Patruno

2017

ApJ

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The accreting millisecond pulsars IGR J00291+5934 and SAX J1808.4-3658 are two compact binaries with very similar orbital parameters. The latter has been observed to evolve on a very short timescale of ∼70 Myr which is more than an order of magnitude shorter than expected. There is an ongoing debate on the possibility that the pulsar spin-down power ablates the companion generating large amount of mass-loss in the system. It is interesting therefore to study whether IGR J00291+5934 does show a similar behaviour as its twin system SAX J1808.4-3658 . In this work we present the first measurement of the orbital period derivative of IGR J00291+5934 . By using XMM-Newton data recorded during the 2015 outburst and adding the previous results of the 2004 and 2008 outbursts, we are able to measure a 90% confidence level upper limit of −5 × 10 −13 <Ṗ b < 6 × 10 −13 s s −1 . This implies that the binary is evolving on a timescale longer than 0.5 Gyr, which is compatible with the expected timescale of mass transfer driven by angular momentum loss via gravitational radiation. We discuss the scenario in which the power loss from magnetic dipole radiation of the neutron star is hitting the companion star. If this model is applied to SAX J1808.4-3658 then the difference in orbital behavior can be ascribed to a different efficiency for the conversion of the spin-down power into energetic relativistic pulsar wind and X-ray/gamma-ray radiation for the two pulsars, with IGR J00291+5934 requiring an extraordinarily low efficiency of less than ∼ 5% to explain the observations. Alternatively, the donor in IGR J00291+5934 is weakly/not magnetized which would suppress the possibility of generating mass-quadrupole variations.

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Section: Resultsmentioning

confidence: 99%

Section: Introductionmentioning

confidence: 99%

The Slow Orbital Evolution of the Accreting Millisecond Pulsar IGR J0029+5934

Patruno

2017

ApJ

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“…IGR J18245-2452, observed as an accreting MSP and an eclipsing RMSP at different times (Papitto et al 2013), is the prototype of this class. A transition to a rotation-powered state during X-ray quiescence has also been proposed for a number of accreting MSPs on the basis of the observed spin-down (Hartman et al , 2009(Hartman et al , 2011Patruno 2010;Papitto et al 2011;Patruno et al 2012b), reprocessed optical emission Campana et al 2004;Di Salvo et al 2008 (Di Salvo et al 2008;Burderi et al 2009;Patruno et al 2012b), even if radio and γ-ray pulsations have not been detected so far (Burgay et al 2003;Iacolina et al 2009Iacolina et al , 2010Xing & Wang 2013). On the other hand, state transitions to an accretion stage have only been observed from eclipsing RMSPs (see above); these sources are the only possible candidates to undergo such fast transitions because the companion star has to spill matter through the inner Lagrangian point of the orbit to do so.…”

Section: Introductionmentioning

confidence: 99%

Spin frequency distributions of binary millisecond pulsars

Papitto

Torres

Rea

et al. 2014

A&A

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Rotation-powered millisecond radio pulsars have been spun up to their present spin period by a 10 8 −10 9 yr long X-ray-bright phase of accretion of matter and angular momentum in a low-to-intermediate mass binary system. Recently, the discovery of transitional pulsars that alternate cyclically between accretion and rotation-powered states on time scales of a few years or shorter, has demonstrated this evolutionary scenario. Here, we present a thorough statistical analysis of the spin distributions of the various classes of millisecond pulsars to assess the evolution of their spin period between the different stages. Accreting sources that showed oscillations exclusively during thermonuclear type I X-ray bursts (nuclear-powered millisecond pulsars) are found to be significantly faster than rotationpowered sources, while accreting sources that possess a magnetosphere and show coherent pulsations (accreting millisecond pulsars) are not. On the other hand, if accreting millisecond pulsars and eclipsing rotation-powered millisecond pulsars form a common class of transitional pulsars, these are shown to have a spin distribution intermediate between the faster nuclear-powered millisecond pulsars and the slower non-eclipsing rotation-powered millisecond pulsars. We interpret these findings in terms of a spin-down due to the decreasing mass-accretion rate during the latest stages of the accretion phase, and in terms of the different orbital evolutionary channels mapped by the various classes of pulsars. We summarize possible instrumental selection effects, showing that even if an unbiased sample of pulsars is still lacking, their influence on the results of the presented analysis is reduced by recent improvements in instrumentation and searching techniques.

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“…Recurrent outbursts were also observed in SAX J1808. 4-3658 (di Salvo et al 2008;Burderi et al 2009;Hartman et al 2009), IGR J00291+5934 (Galloway et al 2005(Galloway et al , 2008Hartman et al 2011;, NGC 6440 X-2 , and Swift J1756.9-2508 . XTE J1751-305 was detected for the first time by RXTE on April 3, 2002 (Markwardt et al 2002, M02, henceforth).…”

Section: Introductionmentioning

confidence: 99%

Secular spin-down of the AMP XTE J1751-305

Riggio¹,

Burderi²,

Salvo³

et al. 2011

A&A

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Context. Of the 13 known accreting millisecond pulsars, only a few have displayed more than one outburst during the RXTE era. 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 RXTE data 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 B PC = 4.0(4) × 10 8 G, for a neutron star mass of 1.4 M , assuming the Friedman Pandharipande Skyrme equation of state.

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Timing of the 2008 outburst of SAX J1808.4–3658 with XMM-Newton: a stable orbital-period derivative over ten years

Cited by 58 publications

References 20 publications

The Slow Orbital Evolution of the Accreting Millisecond Pulsar IGR J0029+5934

The Slow Orbital Evolution of the Accreting Millisecond Pulsar IGR J0029+5934

Spin frequency distributions of binary millisecond pulsars

Secular spin-down of the AMP XTE J1751-305

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