Timing Observations of PSR J1023+0038 During a Low-Mass X-Ray Binary State

Jaodand, Amruta; Archibald, Anne M.; Hessels, J. W. T.; Bogdanov, Slavko; D’Angelo, Caroline; Patruno, A.; Bassa, C. G.; Deller, Adam T.

doi:10.3847/0004-637x/830/2/122

Cited by 86 publications

(170 citation statements)

References 82 publications

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“…X-ray pulsation searches in the redback transitional millisecond pulsar PSRJ1023+0038 (e.g., Archibald et al 2015;Jaodand et al 2016) have established that one can successfully account for such nondeterministic orbital variations by searching over a small deviation in the time of ascending node (T asc ). Therefore, when folding the GBT radio data with X-rayderived ephemerides, we searched both over DM and a ΔT asc value compared to the fiducial ephemeris value.…”

Section: Direct-folding Search With X-ray-derived Ephemerismentioning

confidence: 99%

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Radio Pulse Search and X-Ray Monitoring of SAX J1808.4−3658: What Causes Its Orbital Evolution?

Patruno

Jaodand

Kuiper

et al. 2017

ApJ

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The accreting millisecond X-ray pulsar SAX J1808.4−3658 shows a peculiar orbital evolution that proceeds at a very fast pace. It is important to identify the underlying mechanism responsible for this behavior because it can help to understand how this system evolves and which physical processes (such asmass loss or spin-orbit coupling) are occurring in the binary. It has also been suggested that, when in quiescence, SAX J1808.4−3658 turns on as a radio pulsar, a circumstance that might provide a link between accreting millisecond pulsars and black-widow (BW) radio pulsars. In this work, we report the results of a deep radio pulsation search at 2 GHz using the Green Bank Telescope in 2014 August and an X-ray study of the 2015 outburst with Chandra, SwiftXRT, and INTEGRAL. In quiescence, we detect no radio pulsationsand place the strongest limit to date on the pulsed radio flux density of any accreting millisecond pulsar. We also find that the orbit of SAX J1808.4−3658 continues evolving at a fast pace. We compare the orbital evolution of SAX J1808.4−3658 to that of several other accreting and nonaccreting binaries, including BWs, redbacks, cataclysmic variables, black holes, and neutron stars in lowmass X-ray binaries. We discuss two possible scenarios: either the neutron star has a large moment of inertia and is ablating the donor, generating massloss with an efficiency of 40%, or the donor star has a strong magnetic field of at least 1 kG and is undergoing quasi-cyclic variations due to spin-orbit coupling.

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Section: Direct-folding Search With X-ray-derived Ephemerismentioning

confidence: 99%

“…However, there is at least one situation where, besides the short-term fluctuations discussed above, there is also a decadelong (secular?) variation of the orbit thatcorresponds to an overall shrinkage of the binary orbital separation (see, e.g., PSR J1023+0038; Jaodand et al 2016). …”

Section: Bws and Redbacksmentioning

confidence: 99%

Radio Pulse Search and X-Ray Monitoring of SAX J1808.4−3658: What Causes Its Orbital Evolution?

Patruno

Jaodand

Kuiper

et al. 2017

ApJ

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“…The more recent discovery of transitional millisecond pulsars (tMSPs), which transition back and forth between a rotationpowered MSP and an accretion-powered low-mass X-ray binary (LMXB) state (Archibald et al 2009;Papitto et al 2013;Bassa et al 2014), confirmed the basic recycling model of Alpar et al (1982) and Radhakrishnan & Srinivasan (1982) in which a neutron star is spun up to millisecond spin periods due to the accretion of matter and angular momentum. At the same time, the tMSPs have also raised many questions about the detailed physics of the pulsar recycling process and how efficient it can ultimately be in terms of spinning up neutron stars (e.g., Archibald et al 2015;Deller et al 2015;Papitto et al 2015;Jaodand et al 2016).…”

Section: Introductionmentioning

confidence: 99%

LOFAR Discovery of the Fastest-spinning Millisecond Pulsar in the Galactic Field

Bassa

Pleunis

Hessels

et al. 2017

ApJL

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LOFAR Discovery of the Fastest-spinning Millisecond Pulsar in the Galactic FieldBassa, C.G.; Pleunis, Z.; Hessels, J.W.T.; Ferrara, E.C.; Breton, R.P.; Gusinskaia, N.; Kondratiev, V.I.; Sanidas, S.A.; Nieder, L.; Clark, C.J.; Li, T.; van Amesfoort, A.S.; Burnett, T.H.; Camilo, F.; Michelson, P.F.; Ransom, S.M.; Ray, P.S.; Wood, K. General rights It is not permitted to download or to forward/distribute the text or part of it without the consent of the author(s) and/or copyright holder(s), other than for strictly personal, individual use, unless the work is under an open content license (like Creative Commons). Disclaimer/Complaints regulationsIf you believe that digital publication of certain material infringes any of your rights or (privacy) interests, please let the Library know, stating your reasons. In case of a legitimate complaint, the Library will make the material inaccessible and/or remove it from the website. Please Ask the Library: http://uba.uva.nl/en/contact, or a letter to: Library of the University of Amsterdam, Secretariat, Singel 425, 1012 WP Amsterdam, The Netherlands. You will be contacted as soon as possible. AbstractWe report the discovery of PSR J0952−0607, a 707 Hz binary millisecond pulsar that is now the fastest-spinning neutron star known in the Galactic field (i.e., outside of a globular cluster). PSR J0952−0607 was found using LOFAR at a central observing frequency of 135 MHz, well below the 300 MHz to 3 GHz frequencies typically used in pulsar searches. The discovery is part of an ongoing LOFAR survey targeting unassociated Fermi-Large Area Telescope γ-ray sources. PSR J0952−0607 is in a 6.42 hr orbit around a very low-mass companion, and we identify a strongly variable optical source, modulated at the orbital period of the pulsar, as the binary companion. The light curve of the companion varies by 1.6 mag from ¢ = r 22.2 at maximum to ¢ > r 23.8, indicating that it is irradiated by the pulsar wind. Swift observations place a 3σ upper limit on the -0.3 10 keV X-ray luminosity of <Ĺ 1.1 10 X 31 erg s −1 (using the 0.97 kpc distance inferred from the dispersion measure). Though no eclipses of the radio pulsar are observed, the properties of the system classify it as a black widow binary. The radio pulsed spectrum of PSR J0952−0607, as determined through flux density measurements at 150 and 350 MHz, is extremely steep with a~-3 (where n µ a S ). We discuss the growing evidence that the fastest-spinning radio pulsars have exceptionally steep radio spectra, as well as the prospects for finding more sources like PSR J0952−0607.

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“…While radio pulsations have only been detected from tM-SPs in rotation-powered states, optical and X-ray pulsations have been detected from PSR J1023+0038 in its accreting state (Archibald et al 2015;Jaodand et al 2016;Ambrosino et al 2017;Zampieri et al 2019). Additionally, while γray pulsations have been detected from a large number of nearby MSPs, it remains an open question as to whether or not γ-ray pulsations from a tMSP are also suppressed during accreting states.…”

Section: Pulsation Detection Feasibilitymentioning

confidence: 99%

Optical, X-ray, and γ-ray observations of the candidate transitional millisecond pulsar 4FGL J0427.8-6704

Kennedy

Breton

Clark

et al. 2020

Monthly Notices of the Royal Astronomical Society

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We present an optical, X-ray, and γ-ray study of 1SXPS J042749.2-670434, an eclipsing X-ray binary which has an associated γ-ray counterpart, 4FGL J0427.8-6704. This association has led to the source being classified as a transitional millisecond pulsar (tMSP) in an accreting state. We analyse 10.5 years of Fermi LAT data, and detect a γ-ray eclipse at the same phase as optical and X-ray eclipses at the >5σ level, a significant improvement on the 2.8σlevel of the previous detection. The confirmation of this eclipse solidifies the association between the X-ray source and the γ-ray source, strengthening the tMSP classification. However, analysis of several optical data sets and an X-ray observation do not reveal a change in the source's median brightness over long timescales or a bi-modality on short timescales. Instead, the light curve is dominated by flickering which has a correlation time of 2.6 min alongside a potential quasi-periodic oscillation at ∼21 min. The mass of the primary and secondary star are constrained to be M 1 = 1.43 +0.33 −0.19 M and M 2 = 0.3 +0.17 −0.12 M through modelling of the optical light curve. While this is still consistent with a white dwarf primary, we favour the transitional millisecond pulsar in a low accretion state classification due to the significance of the γ-ray eclipse detection.

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Timing Observations of PSR J1023+0038 During a Low-Mass X-Ray Binary State

Cited by 86 publications

References 82 publications

Radio Pulse Search and X-Ray Monitoring of SAX J1808.4−3658: What Causes Its Orbital Evolution?

Radio Pulse Search and X-Ray Monitoring of SAX J1808.4−3658: What Causes Its Orbital Evolution?

LOFAR Discovery of the Fastest-spinning Millisecond Pulsar in the Galactic Field

Optical, X-ray, and γ-ray observations of the candidate transitional millisecond pulsar 4FGL J0427.8-6704

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