A Radio Pulsar Spinning at 716 Hz

Hessels, J. W. T.; Ransom, S. M.; Stairs, I. H.; Freire, P. C. C.; Kaspi, V. M.; Camilo, F.

doi:10.1126/science.1123430

Cited by 802 publications

(741 citation statements)

References 24 publications

(24 reference statements)

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“…the NS in HMXBs (B ∼ 10 12 G, P ∼ 10 s) like Her X-1 (P = 1.24 s, B = 3 × 10 12 G, see van der Meer et al 2007;Liu et al 2007). With the long-lived accretion phase, the binary accepts sufficient mass from its companion and the NS yields a substantial field decay, as in the case of MSPs (Bhattacharya & van den Heuvel 1991), e.g., the fastest known pulsar PSR J1748-2446 (B ∼ 10 8 G, P = 1.4 ms, see Hessels et al 2006).…”

Section: Influence By Initial Conditionsmentioning

confidence: 99%

Spin period evolution of a recycled pulsar in an accreting binary

Wang

Zhang

Zhao

et al. 2011

A&A

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We investigate the spin period evolutions of recycled pulsars in binary accreting systems. Taking both the accretion induced field decay and spin-up into consideration, we calculate their spin period evolutions influenced by the initial magnetic field strengths, initial spin periods, and accretion rates. The results indicate that the minimum spin period (or maximum spin frequency) of a millisecond pulsar (MSP) is independent of the initial conditions and accretion rate when the neutron star (NS) accretes the mass of ∼0.2 M . The accretion torque with the fastness parameter and gravitational wave (GW) radiation torque may be responsible for the formation of the minimum spin period (maximum spin frequency). The fastest spin frequency (716 Hz) of MSP can be inferred to associate with a critical fastness parameter of about ω c = 0.55. Furthermore, comparisons with the observational data are presented in the field period (B − P) diagram.

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Section: Influence By Initial Conditionsmentioning

confidence: 99%

Spin period evolution of a recycled pulsar in an accreting binary

Wang

Zhang

Zhao

et al. 2011

A&A

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“…As an example, until recently the pulsars in Terzan 5 had the highest dispersion measures (DMs) among all known MSPs (∼240 cm −3 pc), which precluded the detection of fast MSPs. However, improvements in instrumentation now allow the detection of pulsars with very fast spin periods (Ransom et al 2005), including the fastest known, PSR J1748−2446ad (Hessels et al 2006), even for such high DMs.…”

Section: Pulse Periodsmentioning

confidence: 99%

On the disruption of pulsar and X-ray binaries in globular clusters

Verbunt

Freire

2013

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The stellar encounter rate Γ has been shown to be strongly correlated with the number of X-ray binaries in globular clusters (GCs) and also to the number of radio pulsars. However, the pulsar populations in different GCs show remarkably different characteristics: in some GCs the population is dominated by binary systems, in others by single pulsars and exotic systems that result from exchange encounters. In this paper, we describe a second dynamical parameter for GCs, the encounter rate for a single binary, γ. We find that this parameter provides a good characterization of the differences between the pulsar populations of different GCs. The higher γ is for any particular GC, the more isolated pulsars and products of exchange interactions are observed. Furthermore, we also find that slow and "young" pulsars are found almost exclusively in clusters with a high γ; this suggests that these kinds of objects are formed by the disruption of X-ray binaries, thus halting the recycling of a previously dead neutron star. We discuss the implications of this for the nature of young pulsars and for the formation of neutron stars in GCs.

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“…Terzan 5 has the highest stellar interaction rate than any cluster in the Galaxy (Verbunt & Hut 1987;Heinke et al 2003a;Bahramian et al 2013). This reflects into the largest population known of millisecond radio pulsars (34; Ransom et al 2005;Hessels et al 2006), and in at least 50 X-ray sources, including a dozen likely quiescent LMXBs (Heinke et al 2006). The populations of millisecond radio pulsars and LMXBs are linked from an evolutionary point of view, as mass accretion in a LMXB is expected to speed up the rotation of a NS down to a spin period of a few milliseconds (Alpar et al 1982).…”

Section: Introductionmentioning

confidence: 99%

XMM-Newtonand INTEGRAL view of the hard state of EXO 1745−248 during its 2015 outburst

Matranga

Papitto

Salvo

et al. 2017

A&A

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Context. Transient low-mass X-ray binaries (LMXBs) often show outbursts lasting typically a few-weeks and characterized by a high X-ray luminosity (L x ≈ 10 36 − 10 38 erg s −1 ), while for most of the time they are found in X-ray quiescence (L X ≈ 10 31 − 10 33 erg s −1 ). EXO 1745-248 is one of them. Aims. The broad-band coverage, and the sensitivity of instrumet on board of XMM-Newton and INTEGRAL, offers the opportunity to characterize the hard X-ray spectrum during EXO 1745-248 outburst. Methods. In this paper we report on quasi-simultaneous XMM-Newton and INTEGRAL observations of the X-ray transient EXO 1745-248 located in the globular cluster Terzan 5, performed ten days after the beginning of the outburst (on 2015 March 16th) shown by the source between March and June 2015. The source was caught in a hard state, emitting a 0.8-100 keV luminosity of ≃ 10 37 erg s −1 . Results. The spectral continuum was dominated by thermal Comptonization of seed photons with temperature kT in ≃ 1.3 keV, by a cloud with moderate optical depth τ ≃ 2 and electron temperature kT e ≃ 40 keV. A weaker soft thermal component at temperature kT th ≃ 0.6-0.7 keV and compatible with a fraction of the neutron star radius was also detected. A rich emission line spectrum was observed by the EPIC-pn on-board XMM-Newton; features at energies compatible with K-α transitions of ionized sulfur, argon, calcium and iron were detected, with a broadness compatible with either thermal Compton broadening or Doppler broadening in the inner parts of an accretion disk truncated at 20 ± 6 gravitational radii from the neutron star. Strikingly, at least one narrow emission line ascribed to neutral or mildly ionized iron is needed to model the prominent emission complex detected between 5.5 and 7.5 keV. The different ionization state and broadness suggest an origin in a region located farther from the neutron star than where the other emission lines are produced. Seven consecutive type-I bursts were detected during the XMM-Newton observation, none of which showed hints of photospheric radius expansion. A thorough search for coherent pulsations from the EPIC-pn light curve did not result in any significant detection. Upper limits ranging from a few to 15% on the signal amplitude were set, depending on the unknown spin and orbital parameters of the system.

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A Radio Pulsar Spinning at 716 Hz

Cited by 802 publications

References 24 publications

Spin period evolution of a recycled pulsar in an accreting binary

Spin period evolution of a recycled pulsar in an accreting binary

On the disruption of pulsar and X-ray binaries in globular clusters

XMM-Newtonand INTEGRAL view of the hard state of EXO 1745−248 during its 2015 outburst

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