An ultraluminous nascent millisecond pulsar

Kluźniak, W.; Lasota, Jean–Pierre

doi:10.1093/mnrasl/slu200

Cited by 71 publications

(78 citation statements)

References 39 publications

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“…However, other authors have instead suggested that the magnetic field is much lower (potentially as low as B ∼ 10 9 G) based on the ratio of the spin-up rate to the luminosity, which is an order of magnitude lower than typical X-ray pulsars (e.g. Kluźniak & Lasota 2015). These authors argue that a disk truncated at a large radius (close to the co-rotation radius, Rco, as would occur for a high-B field system; Rco is the point at which the material in the disc co-rotates with the neutron star, and RM < Rco is required for strong accretion to occur) would not provide the required lever arm to power the observed spin up.…”

Section: Introductionmentioning

confidence: 91%

Super-Eddington accretion on to the neutron star NGC 7793 P13: Broad-band X-ray spectroscopy and ultraluminous X-ray sources

Walton

Fürst

Harrison

et al. 2017

Monthly Notices of the Royal Astronomical Society

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We present a detailed, broadband X-ray spectral analysis of the ULX pulsar NGC 7793 P13, a known super-Eddington source, utilizing data from the XMM-Newton, NuSTAR and Chandra observatories. The broadband XMM-Newton+NuSTAR spectrum of P13 is qualitatively similar to the rest of the ULX sample with broadband coverage, suggesting that additional ULXs in the known population may host neutron star accretors. Through time-averaged, phaseresolved and multi-epoch studies, we find that two non-pulsed thermal blackbody components with temperatures ∼0.5 and 1.5 keV are required to fit the data below 10 keV, in addition to a third continuum component which extends to higher energies and is associated with the pulsed emission from the accretion column. The characteristic radii of the thermal components appear to be comparable, and are too large to be associated with the neutron star itself, so the need for two components likely indicates the accretion flow outside the magnetosphere is complex. We suggest a scenario in which the thick inner disc expected for super-Eddington accretion begins to form, but is terminated by the neutron star's magnetic field soon after its onset, implying a limit of B 6 × 10 12 G for the dipolar component of the central neutron star's magnetic field. Evidence of similar termination of the disc in other sources may offer a further means of identifying additional neutron star ULXs. Finally, we examine the spectrum exhibited by P13 during one of its unusual 'off' states. These data require both a hard powerlaw component, suggesting residual accretion onto the neutron star, and emission from a thermal plasma, which we argue is likely associated with the P13 system.

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Section: Introductionmentioning

confidence: 91%

Super-Eddington accretion on to the neutron star NGC 7793 P13: Broad-band X-ray spectroscopy and ultraluminous X-ray sources

Walton

Fürst

Harrison

et al. 2017

Monthly Notices of the Royal Astronomical Society

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“…The recent discovery that a number of ultra-luminous X-ray sources (ULXs: M82 X-2, NGC 7793 P13 and NGC 5907) are pulsating NSs (Bachetti et al 2014;Israel et al 2017b;Fürst et al 2016;Israel et al 2017a) has lead to the suggestion that ULXs might be HMXBs (Ekşi et al 2015;Kluźniak & Lasota 2015;Shao & Li 2015;Mushtukov et al 2015), including BeHMXBs (Karino & Miller 2016;Christodoulou et al 2017), and which could therefore suggest that some ULXs might potentially lead to the production DNS systems.…”

Section: Ulxs: Origin and Connection To Dns Progenitors?mentioning

confidence: 99%

Formation of Double Neutron Star Systems

Tauris

Krämer

Freire

et al. 2017

ApJ

602

684

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Double neutron star (DNS) systems represent extreme physical objects and the endpoint of an exotic journey of stellar evolution and binary interactions. Large numbers of DNS systems and their mergers are anticipated to be discovered using the Square-Kilometre-Array searching for radio pulsars and high-frequency gravitational wave detectors (LIGO/VIRGO), respectively. Here we discuss all key properties of DNS systems, as well as selection effects, and combine the latest observational data with new theoretical progress on various physical processes with the aim of advancing our knowledge on their formation. We examine key interactions of their progenitor systems and evaluate their accretion history during the high-mass X-ray binary stage, the common envelope phase and the subsequent Case BB mass transfer, and argue that the first-formed NSs have accreted at most ∼ 0.02 M ⊙ . We investigate DNS masses, spins and velocities, and in particular correlations between spin period, orbital period and eccentricity. Numerous Monte Carlo simulations of the second supernova (SN) events are performed to extrapolate pre-SN stellar properties and probe the explosions. All known close-orbit DNS systems are consistent with ultra-stripped exploding stars. Although their resulting NS kicks are often small, we demonstrate a large spread in kick magnitudes which may, in general, depend on the past interaction history of the exploding star and thus correlate with the NS mass. We analyze and discuss NS kick directions based on our SN simulations. Finally, we discuss the terminal evolution of close-orbit DNS systems until they merge and possibly produce a short γ-ray burst.

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“…Christodoulou et al 2014). This source has also been proposed as an alternative path for the formation of millisecond pulsars (Kluźniak and Lasota 2015).…”

Section: M82 -A Cradle Of Exceptionsmentioning

confidence: 99%

Ultraluminous X‐ray sources: Three exciting years

Bachetti

2016

Astron Nachr

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The extreme extragalactic sources known as Ultraluminous X-ray Sources (ULX) represent a unique testing environment for compact objects population studies and the accretion process. Their nature has long been disputed. Their luminosity, well above the Eddington luminosity for a stellar-mass black hole, can imply the presence of an intermediate-mass black hole or a stellar black hole accreting above the Eddington limit. Both these interpretations are important to understand better the accretion process and the evolution of massive black holes. The last few years have seen a dramatic improvement of our knowledge of these sources. In particular, the super-Eddington interpretation for the bulk of the ULX population has gained a strong consensus. Nonetheless, exceptions to this general trend do exist, and in particular one ULX was shown to be a neutron star, and another was shown to be a very likely IMBH candidate. In this paper, I will review the progress done in the last few years.

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An ultraluminous nascent millisecond pulsar

Cited by 71 publications

References 39 publications

Super-Eddington accretion on to the neutron star NGC 7793 P13: Broad-band X-ray spectroscopy and ultraluminous X-ray sources

Super-Eddington accretion on to the neutron star NGC 7793 P13: Broad-band X-ray spectroscopy and ultraluminous X-ray sources

Formation of Double Neutron Star Systems

Ultraluminous X‐ray sources: Three exciting years

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