A Radio Pulsar/X-ray Binary Link

Archibald, Anne M.; Stairs, I. H.; Ransom, S. M.; Kaspi, V. M.; Kondratiev, V. I.; Lorimer, D. R.; McLaughlin, M. A.; Boyles, J.; Hessels, J. W. T.; Lynch, R.; Leeuwen, J. van; Roberts, M. S. E.; Jenet, F. A.; Champion, D. J.; Rosen, Rachel A.; Barlow, B. N.; Dunlap, B. H.; Remillard, Ronald A.

doi:10.1126/science.1172740

Cited by 549 publications

(660 citation statements)

References 22 publications

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“…Of course, since the discovery of the first eclipsing pulsars we know of systems where mass transfer (loss from the companion) occurs with no accretion onto the neutron star, however this is an unlikely scenario for the binary at hand. Although, perhaps, at some point in time the pulsar could turn on in the radio, (i.e., become a radio pulsar if the mass transfer rate temporarily drops) as predicted theoretically (Kluźniak et al 1988) and recently observed (e.g., Archibald et al 2009;Bassa et al 2014), it would take a very powerful radio pulsar indeed to expel from the system matter transferred at such a prodigious rate. Note that the known eclipsing pulsars that ablate their companions are in fact millisecond pulsars, and their companions have fairly low masses.…”

Section: An Ultraluminous Accreting Millisecond Pulsarmentioning

confidence: 99%

An ultraluminous nascent millisecond pulsar

Kluźniak

Lasota

2015

Monthly Notices of the Royal Astronomical Society: Letters

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If the ultraluminous source (ULX) M82 X-2 sustains its measured spin-up value oḟ ν = 10 −10 s −2 , it will become a millisecond pulsar in less than 10 5 yr. The observed (isotropic) luminosity of 10 40 erg/s also supports the notion that the neutron star will spin up to a millisecond period upon accreting about 0.1 M ⊙ -the reported hard X-ray luminosity of this ULX, together with the spin-up value, implies torques consistent with the accretion disc extending down to the vicinity of the stellar surface, as expected for low values of the stellar dipole magnetic field (B 10 9 G). This suggests a new channel of millisecond pulsar formation-in high-mass X-ray binaries (HMXBs)-and may have implications for studies of gravitational waves, and possibly for the formation of low-mass black holes through accretion-induced collapse.

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Section: An Ultraluminous Accreting Millisecond Pulsarmentioning

confidence: 99%

An ultraluminous nascent millisecond pulsar

Kluźniak

Lasota

2015

Monthly Notices of the Royal Astronomical Society: Letters

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“…In this case the magnetosphere should be devoid of matter and the radio pulsar mechanism should turn on with a strong pulsar wind preventing further accretion (see e.g., Stella et al 1994;Burderi et al 2001). This is what is currently thought to occur in the radio-pulsar phase of the three transitional pulsars recently discovered (Archibald et al 2009;Papitto et al 2013;Bassa et al 2014;Patruno et al 2014;Roy et al 2014Roy et al , 2015Stappers et al 2014) and in the quiescence phase of SAX J1808.4−3658 (Homer et al 2001;Burderi et al 2003;). The fact that in SAX J1808.4 −3658 the X-ray luminosity increases by three orders of magnitude right after reaching the luminosity minima on a very fast timescale of 1-2 days (see Figures 2 and 3) suggests that the radio pulsar mechanism does not turn on, although a very rapid switch cannot be excluded at the moment.…”

Section: Accretion Flow Geometrymentioning

confidence: 99%

The Reflares and Outburst Evolution in the Accreting Millisecond Pulsar Sax J1808.4–3658: A Disk Truncated Near Co-Rotation?

Patruno

Maitra

Curran

et al. 2016

ApJ

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The accreting millisecond X-ray pulsar SAX J1808.4-3658 shows peculiar low luminosity states known as "reflares" after the end of the main outburst. During this phase the X-ray luminosity of the source varies by up to three orders of magnitude in less than 1-2 days. The lowest X-ray luminosity observed reaches a value of 10 erg s 32 1 -, only a factor of a few brighter than its typical quiescent level. We investigate the 2008 and 2005 reflaring state of SAX J1808.4-3658 to determine whether there is any evidence for a change in the accretion flow with respect to the main outburst. We perform a multiwavelength photometric and spectral study of the 2005 and 2008 reflares with data collected during an observational campaign covering the near-infrared, optical, ultra-violet and X-ray band. We find that the NIR/optical/UV emission, expected to come from the outer accretion disk, shows variations in luminosity over an order of magnitude. The corresponding X-ray luminosity variations are instead much deeper, spanning about 2-3 orders of magnitude. The X-ray spectral state observed during the reflares does not change substantially with X-ray luminosity, indicating a rather stable configuration of the accretion flow. We investigate the most likely configuration of the innermost regions of the accretion flow and we infer an accretion disk truncated at or near the co-rotation radius. We interpret these findings as due to either a strong outflow (due to a propeller effect) or a trapped disk (with limited/no outflow) in the inner regions of the accretion flow.

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“…Beccari et al (2014) use Hα, V and I photometry to calculate Hα EWs of 28Å and 50Å for the quiescent NS LMXBs W125 and W58/X5 in the globular cluster 47 Tuc. Finally, three systems (PSR J1023+0038, M28I=IGR J18245-2452, and XSS J12270-4859) swing between radio pulsations and active accretion (Archibald et al 2009;Papitto et al 2013;Bassa et al 2014). These three systems show no evidence of Hα emission (or other disc signatures) when in their radio pulsar state (Thorstensen & Armstrong 2005;Pallanca et al 2013;Bassa et al 2014), but show Hα EWs of 14-19Å (Szkody et al 2003;Halpern et al 2013), 72±5 A (Pallanca et al 2013), and 10-20Å (Masetti et al 2006;Pretorius 2009), respectively, when pulsations stop, and accretion, or a pulsar wind shock, produces low-level X-ray emission (LX ∼ 10 33 ergs/s).…”

Section: Ngc 6397: Hst Datamentioning

confidence: 99%

Improved mass and radius constraints for quiescent neutron stars in ω Cen and NGC 6397

Heinke¹,

Cohn²,

Lugger³

et al. 2014

Monthly Notices of the Royal Astronomical Society

111

155

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We use Chandra and XMM-Newton observations of the globular clusters ω Cen and NGC 6397 to measure the spectrum of their quiescent neutron stars (NSs), and thus to constrain the allowed ranges of mass and radius for each. We also use Hubble Space Telescope photometry of NGC 6397 to identify a potential optical companion to the quiescent NS, and find evidence that the companion lacks hydrogen. We carefully consider a number of systematic problems, and show that the choices of atmospheric composition, interstellar medium abundances, and cluster distances can have important effects on the inferred NS mass and radius. We find that for typical NS masses, the radii of both NSs are consistent with the 10 − 13 km range favored by recent nuclear physics experiments. This removes the evidence suggested by Guillot and collaborators for an unusually small NS radius, which relied upon the small inferred radius of the NGC 6397 NS.

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A Radio Pulsar/X-ray Binary Link

Cited by 549 publications

References 22 publications

An ultraluminous nascent millisecond pulsar

An ultraluminous nascent millisecond pulsar

The Reflares and Outburst Evolution in the Accreting Millisecond Pulsar Sax J1808.4–3658: A Disk Truncated Near Co-Rotation?

Improved mass and radius constraints for quiescent neutron stars in ω Cen and NGC 6397

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