The Book of Judges / Barry G Webb G; and Judges / Serge Frolov

Jonker, Louis

doi:10.7833/113-0-734

Cited by 35 publications

(56 citation statements)

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“…Note that the uncertainties on the luminosities due to distance and flux measurement uncertainties (e.g. Jonker & Nelemans 2004 for the distance uncertainties) are not included. tion disc contribution of 50 per cent to the R-band luminosity and an M2 V companion star, we derive a distance of 5.9 kpc, which we round to 6 kpc.…”

Section: Discussionmentioning

confidence: 99%

“…the upper limit to the radio luminosity for XTE J1118+480; cf. Miller-Jones et al 2011a), although there is uncertainty on the normalization due to distance uncertainties (Jonker & Nelemans 2004;). Nevertheless, our radio non-detection for an X-ray luminosity of 3.3 × 10 32 to 1.3 × 10 33 erg s −1 for a distance of 4 and 8 kpc, respectively, is constraining.…”

Section: Discussionmentioning

confidence: 99%

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The black hole candidate MAXI J1659-152 in and towards quiescence in X-ray and radio

Jonker

Miller-Jones

Homan

et al. 2012

Monthly Notices of the Royal Astronomical Society

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In this paper we report on Expanded Very Large Array radio and Chandra and Swift X‐ray observations of the outburst decay of the transient black hole candidate MAXI J1659–152 in 2011. We discuss the distance to the source taking the high inclination into account and conclude that the source distance is probably 6 ± 2 kpc. The lowest observed flux corresponds to a luminosity of erg s−1. This, together with the orbital period of 2.4 h reported in the literature, suggests that the quiescent X‐ray luminosity is higher than predicted on the basis of the orbital period–quiescent X‐ray luminosity relationship. It is more in line with that expected for a neutron star, although the outburst spectral and timing properties reported in the literature strongly suggest that MAXI J1659–152 harbours a black hole. This conclusion is subject to confirmation of the lowest observed flux as the quiescent flux. The relation between the accretion and ejection mechanisms can be studied using the observed correlation between the radio and X‐ray luminosities as these evolve over an outburst. We determine the behaviour of MAXI J1659–152 in the radio–X‐ray diagram at low X‐ray luminosities using the observations reported in this paper and at high X‐ray luminosities using values reported in the literature. At high X‐ray luminosities, the source lies closer to the sources that follow a correlation index steeper than 0.6–0.7. However, when compared to other sources that follow a steeper correlation index, the X‐ray luminosity in MAXI J1659–152 is also lower. The latter can potentially be explained by the high inclination of MAXI J1659–152 if the X‐ray emission comes from close to the source and the radio emission is originating in a more extended region. However, it is probable that the source was not in the canonical low‐hard state during these radio observations and this may affect the behaviour of the source as well. At intermediate X‐ray luminosities, the source makes the transition from the radio underluminous sources in the direction of the relation traced by the ‘standard’ correlation similar to what has been reported for H 1743−322 in the literature. However, MAXI J1659–152 remains underluminous with respect to this ‘standard’ correlation.

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Section: Discussionmentioning

confidence: 99%

Section: Discussionmentioning

confidence: 99%

The black hole candidate MAXI J1659-152 in and towards quiescence in X-ray and radio

Jonker

Miller-Jones

Homan

et al. 2012

Monthly Notices of the Royal Astronomical Society

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“…Column 5: the orbital period of the system. Unless otherwise stated, parameters are from Liu et al (2005Liu et al ( , 2006Liu et al ( , 2007 and Jonker & Nelemans (2004). Note.…”

Section: Model Fittingmentioning

confidence: 99%

Revisiting a fundamental test of the disc instability model for X-ray binaries

Coriat

Fender

Dubus

2012

Monthly Notices of the Royal Astronomical Society

142

137

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We revisit a core prediction of the disc instability model (DIM) applied to X‐ray binaries. The model predicts the existence of a critical mass‐transfer rate, which depends on disc size, separating transient and persistent systems. We therefore selected a sample of 52 persistent and transient neutron star and black hole X‐ray binaries and verified if the observed persistent (transient) systems do lie in the appropriate stable (unstable) region of parameter space predicted by the model. We find that, despite the significant uncertainties inherent to these kinds of studies, the data are in very good agreement with the theoretical expectations. We then discuss some individual cases that do not clearly fit into this main conclusion. Finally, we introduce the transientness parameter as a measure of the activity of a source and show a clear trend of the average outburst recurrence time to decrease with transientness in agreement with the DIM predictions. We therefore conclude that, despite difficulties in reproducing the complex details of the light curves, the DIM succeeds in explaining the global behaviour of X‐ray binaries averaged over a long enough period of time.

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“…BHs can be studied via interacting X-ray binaries which contain them. There are several known X-ray binaries which are known to contain BHs or contain BH candidates (Jonker & Nelemans 2004;Özel et al 2010). In these systems, the massive primary has evolved to form a BH via a core-collapse SN and material is currently flowing from the lower mass secondary (typically via Roche lobe overflow -RLO) on to the BH via an accretion disc (for a detailed review on the evolution of compact binaries see Tauris & van den Heuvel 2006).…”

Section: Introductionmentioning

confidence: 99%

“…In this paper, we consider the population of BH X-ray binaries as a whole (following the approach of White & van Paradijs 1996;Jonker & Nelemans 2004;Zuo, Li & Liu 2008) rather than considering the kinematics of an individual system. We synthesize a population of BH low-mass X-ray binaries (BH-LMXBs), using various NK distributions, and integrating the systems within the Galactic potential.…”

Section: Introductionmentioning

confidence: 99%

Investigating stellar-mass black hole kicks

Repetto

Davies²,

Sigurd̵sson

2012

Monthly Notices of the Royal Astronomical Society

226

223

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We investigate whether stellar-mass black holes have to receive natal kicks in order to explain the observed distribution of low-mass X-ray binaries containing black holes within our Galaxy. Such binaries are the product of binary evolution, where the massive primary has exploded forming a stellar-mass black hole, probably after a common envelope phase where the system contracted down to separations of order 10-30 Rsun. We perform population synthesis calculations of these binaries, applying both kicks due to supernova mass-loss and natal kicks to the newly-formed black hole. We then integrate the trajectories of the binary systems within the Galactic potential. We find that natal kicks are in fact necessary to reach the large distances above the Galactic plane achieved by some binaries. Further, we find that the distribution of natal kicks would seem to be similar to that of neutron stars, rather than one where the kick velocities are reduced by the ratio of black hole to neutron-star mass (i.e. where the kicks have the same momentum). This result is somewhat surprising; in many pictures of stellar-mass black-hole formation, one might have expected black holes to receive kicks having the same momentum (rather than the same speed) as those given to neutron stars.Comment: 13 pages, 8 figures, 4 tables. Accepted for publication in MNRA

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The Book of Judges / Barry G Webb G; and Judges / Serge Frolov

Cited by 35 publications

References 0 publications

The black hole candidate MAXI J1659-152 in and towards quiescence in X-ray and radio

The black hole candidate MAXI J1659-152 in and towards quiescence in X-ray and radio

Revisiting a fundamental test of the disc instability model for X-ray binaries

Investigating stellar-mass black hole kicks

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