The influence of spin on jet power in neutron star X-ray binaries

Migliari, S.; Miller-Jones, J. C. A.; Russell, D. M.

doi:10.1111/j.1365-2966.2011.18868.x

Cited by 49 publications

(50 citation statements)

References 77 publications

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“…Meanwhile, as discussed in Section 4.2 for the 'propeller' effect, theoretically, the spin of NS plays a very important role in the formation and the power of the jet. The observational hint for the correlation between the spin frequency and the jet power in NSs was confirmed by Migliari et al (2011). A more systematic study of the effects of the spin of NS on the X-ray emission from the ADAF and the radio emission from the jet (jet power) for the radio/X-ray correlation in NSs will be continued in the future work.…”

Section: The Effect Of the Ns Spinmentioning

confidence: 62%

A model for the radio/X-ray correlation in three neutron star low-mass X-ray binaries 4U 1728-34, Aql X-1ad, and EXO 1745-248

Qiao

Liu

2019

Monthly Notices of the Royal Astronomical Society

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Observationally, for neutron star low-mass X-ray binaries, so far, the correlation between the radio luminosity L R and the X-ray luminosity L X , i.e., L R ∝ L β X , has been reasonably wellestablished only in three sources 4U 1728-34, Aql X-1 and EXO 1745-248 in their hard state. The slope β of the radio/X-ray correlation of the three sources is different, i.e., β ∼ 1.4 for 4U 1728-34, β ∼ 0.4 for Aql X-1, and β ∼ 1.6 for EXO 1745-248. In this paper, for the first time we explain the different radio/X-ray correlation of 4U 1728-34, Aql X-1 and EXO 1745-248 with the coupled advection-dominated accretion (ADAF)-jet model respectively. We calculate the emergent spectrum of the ADAF-jet model for L X and L R at differentṁ (ṁ =Ṁ/Ṁ Edd ), adjusting η (η ≡Ṁ jet /Ṁ, describing the fraction of the accreted matter in the ADAF transfered vertically forming the jet) to fit the observed radio/X-ray correlations. Then we derive a fitting formula of η as a function ofṁ for 4U 1728-34, Aql X-1 and EXO 1745-248 respectively. If the relation between η andṁ can be extrapolated down to a lower value ofṁ, we find that in a wide range ofṁ, the value of η in Aql X-1 is greater than that of in 4U 1728-34 and EXO 1745-248, implying that Aql X-1 may have a relatively stronger large-scale magnetic field, which is supported by the discovery of the coherent millisecond X-ray pulsation in Aql X-1.

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Section: The Effect Of the Ns Spinmentioning

confidence: 62%

A model for the radio/X-ray correlation in three neutron star low-mass X-ray binaries 4U 1728-34, Aql X-1ad, and EXO 1745-248

Qiao

Liu

2019

Monthly Notices of the Royal Astronomical Society

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“…Tetarenko et al (2018) investigated the influence of orbital period in ultra-compact NS-LMXBs on radio brightness, but found no correlation. Similarly, Migliari et al (2011) found no correlation between NS spin rate and radio brightness, and Russell et al (2018a) suggested that the spin did not account for the high radio luminosity of IGR J17591−2342. Indeed, we find there is no clear difference in the spin rates of "radio-luminous" AMXPs (IGR J17591−2342, IGR J17379−3747, XTE J0929−314 and M28I) and the rest of the population.…”

Section: Radio-x-ray Relationmentioning

confidence: 98%

Radio and X-ray monitoring of the accreting millisecond X-ray pulsar IGR J17591−2342 in outburst

Gusinskaia

Russell

Hessels

et al. 2019

Monthly Notices of the Royal Astronomical Society

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IGR J17591−2342 is a new accreting millisecond X-ray pulsar (AMXP) that was recently discovered in outburst in 2018. Early observations revealed that the source's radio emission is brighter than that of any other known neutron star low-mass X-ray binary (NS-LMXB) at comparable X-ray luminosity, and assuming its likely ∼ > 6 kpc distance. It is comparably radio bright to black hole LMXBs at similar X-ray luminosities. In this work, we present the results of our extensive radio and X-ray monitoring campaign of the 2018 outburst of IGR J17591−2342. In total we collected 10 quasisimultaneous radio (VLA, ATCA) and X-ray (Swift-XRT) observations, which make IGR J17591−2342 one of the best-sampled NS-LMXBs. We use these to fit a power-law correlation index β = 0.37 +0.42 −0.40 between observed radio and X-ray luminosities (L R ∝ L X β ). However, our monitoring revealed a large scatter in IGR J17591−2342's radio luminosity (at a similar X-ray luminosity, L X ∼ 10 36 erg s −1 , and spectral state), with L R ∼ 4×10 29 erg s −1 during the first three reported observations, and up to a factor of 4 lower L R during later radio observations. Nonetheless, the average radio luminosity of IGR J17591−2342 is still one of the highest among NS-LMXBs, and we discuss possible reasons for the wide range of radio luminosities observed in such systems during outburst. We found no evidence for radio pulsations from IGR J17591−2342 in our Green Bank Telescope observations performed shortly after the source returned to quiescence. Nonetheless, we cannot rule out that IGR J17591−2342 becomes a radio millisecond pulsar during quiescence.

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“…The blue circles represent NS systems in the hard state (Rutledge et al 1998;Moore et al 2000;Migliari et al 2003Migliari et al , 2010Migliari et al , 2011Migliari & Fender 2006;Tudose et al 2009;Miller-Jones et al 2010;Tetarenko et al 2016a). Green triangles and pink stars show the binary transitional millisecond pulsar (Hill et al 2011;Papitto et al 2013;Deller et al 2015) and accreting millisecond pulsar (Gaensler et al 1999;Rupen et al 2002;Fender et al 2004b;Pooley 2004;Rupen et al 2005;Migliari et al 2011) systems, respectively. The purple diamonds show the CVs, AE Aqr (Eracleous et al 1991;Abada-Simon et al 1993) and SS Cyg (Russell et al 2016), during bright flare/outburst periods in each source.…”

Section: Optical Analysismentioning

confidence: 99%

The First Low-Mass Black Hole X-Ray Binary Identified in Quiescence Outside of a Globular Cluster

Tetarenko

Bahramian

Arnason

et al. 2016

ApJ

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The observed relation between the X-ray and radio properties of low-luminosity accreting black holes (BHs) has enabled the identification of multiple candidate black hole X-ray binaries (BHXBs) in globular clusters (GCs). Here, we report an identification of the radio source VLA J213002.08+120904 (aka M15 S2), recently reported in Kirsten et al., as a BHXB candidate. They showed that the parallax of this flat-spectrum variable radio source indicates a -+ 2.2 0.3 0.5 kpc distance, which identifies it as lying in the foreground of the GC M15. We determine the radio characteristics of this source and place a deep limit on the X-ray luminosity of ∼4 × 10 29 erg s −1 . Furthermore, we astrometrically identify a faint red stellar counterpart in archival Hubble images with colors consistent with a foreground star; at 2.2 kpc, its inferred mass is 0.1-0.2 M e . We rule out that this object is a pulsar, neutron star X-ray binary, cataclysmic variable, or planetary nebula, concluding that VLA J213002.08+120904 is the first accreting BHXB candidate discovered in quiescence outside of a GC. Given the relatively small area over which parallax studies of radio sources have been performed, this discovery suggests a much larger population of quiescent BHXBs in our Galaxy, 2.6 × 10 4 -1.7 × 10 8 BHXBs at 3σ confidence, than has been previously estimated (∼10 2 -10 4 ) through population synthesis.

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The influence of spin on jet power in neutron star X-ray binaries

Cited by 49 publications

References 77 publications

A model for the radio/X-ray correlation in three neutron star low-mass X-ray binaries 4U 1728-34, Aql X-1ad, and EXO 1745-248

A model for the radio/X-ray correlation in three neutron star low-mass X-ray binaries 4U 1728-34, Aql X-1ad, and EXO 1745-248

Radio and X-ray monitoring of the accreting millisecond X-ray pulsar IGR J17591−2342 in outburst

The First Low-Mass Black Hole X-Ray Binary Identified in Quiescence Outside of a Globular Cluster

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