The quiescent light curve and the evolutionary state of GRO J1655-40

Beer, Martin E.; Podsiadlowski, Philipp

doi:10.1046/j.1365-8711.2002.05189.x

Cited by 129 publications

(171 citation statements)

References 38 publications

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“…Adopting the distance of 3.2 kpc by Hjellming & Rupen (1995), and an average reddening law (R V = 3.2), they obtain E(B − V) = 1.25 ± 0.17 in agreement with previous publications. Beer & Podsiadlowski (2002) reanalyzed the lightcurve in quiescence obtained by Orosz & Bailyn (1997). In their models, the distance is said to be a free parameter, although it is not clear if this parameter has been allowed to go as low as 1.0 kpc.…”

Section: The Problem Of the Distancementioning

confidence: 99%

On the distance of GRO J1655-40

Foellmi

Depagne

Dall³

et al. 2006

A&A

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Aims. We challenge the accepted distance of 3.2 kpc of GRO J1655-40. We present VLT-UVES spectroscopic observations to estimate the absorption toward the source, and determine a maximum distance of GRO J1655-40. Methods. We show that the accepted value of 3.2 kpc is taken for granted by many authors. We retrieved in the ESO archive UVES spectra taken in April 2004 when GRO J1655-40 was in quiescence to determine the spectral type of the secondary star. For the first time we build a flux-calibrated mean (UVES) spectrum of GRO J1655-40 and compare its observed flux to that of five nearby stars of similar spectral types. We strengthen our results with the traditional pair method, using published photometric data of the comparison stars. Results. We show that the distance of 3.2 kpc is questionable. We determine a spectral type F6IV for the secondary star. We demonstrate in details that the distance of GRO J1655-40 must be smaller than 1.7 kpc. Conclusions. The runaway black hole GRO J1655-40 could be associated with the open cluster NGC 6242 which is located at 1.0 ± 0.1 kpc from the Sun. At D ≤ 1.7 kpc the jets are not a superluminal, and GRO J1655-40 becomes one of the closest known black holes to the Sun.

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Section: The Problem Of the Distancementioning

confidence: 99%

On the distance of GRO J1655-40

Foellmi

Depagne

Dall³

et al. 2006

A&A

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“…Using the same arguments as in the case of XTE J1819-254, we reset this lower limit to -75 km s 1 . For XTE J1550-564, XTE J1819-254 and 4U 1543-47, we keep original Repetto et al (2012) estimates, but we mark our modest revisions both in Table 7 ) adopted from Beer & Podsiadlowski (2002). We chose this model as this mass was later confirmed by X-ray timing analysis (Motta et al 2014;   M 5.31 0.07…”

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confidence: 99%

Compact Binary Merger Rates: Comparison With Ligo/Virgo Upper Limits

Belczyński

Repetto

Holz

et al. 2016

ApJ

257

281

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We compare evolutionary predictions of double compact object merger rate densities with initial and forthcoming LIGO/Virgo upper limits. We find that: (i) Due to the cosmological reach of advanced detectors, current conversion methods of population synthesis predictions into merger rate densities are insufficient. (ii) Our optimistic models are a factor of 18 below the initial LIGO/Virgo upper limits for BH-BH systems, indicating that a modest increase in observational sensitivity (by a factor of ∼2.5) may bring the first detections or first gravitational wave constraints on binary evolution. (iii) Stellar-origin massive BH-BH mergers should dominate event rates in advanced LIGO/Virgo and can be detected out to redshift z;2 with templates including inspiral, merger, and ringdown. Normal stars (<  M 150) can produce such mergers with total redshifted mass up to. (iv) High black hole (BH) natal kicks can severely limit the formation of massive BH-BH systems (both in isolated binary and in dynamical dense cluster evolution), and thus would eliminate detection of these systems even at full advanced LIGO/Virgo sensitivity. We find that low and high BH natal kicks are allowed by current observational electromagnetic constraints. (v) The majority of our models yield detections of all types of mergers (NS-NS, BH-NS, BH-BH) with advanced detectors. Numerous massive BH-BH merger detections will indicate small (if any) natal kicks for massive BHs.

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“…This makes it quite difficult for a significant mass fraction of iron to have escaped from the collapsing matter in the SN event because iron is formed in the inner layers of the star. Israelian et al (1999) found in Nova Scorpii 94 that while -elements were enhanced Fe was not, in spite of the lower mass of the compact object (5:4 AE 0:3 M ; Beer & Podsiadlowski 2002) than that in A0620À00. Thus, the SN may not eject any iron, and it therefore seems quite plausible that the slightly higher than solar Fe abundance of the secondary star in A0620À00 reflects its primordial value.…”

Section: Evv Olutionary Scenariomentioning

confidence: 95%

Chemical Abundances in the Secondary Star in the Black Hole Binary A0620−00

Hernández

Rebolo

Israelian

et al. 2004

ApJ

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Using a high-resolution spectrum of the secondary star in the black hole binary A0620À00, we have derived the stellar parameters and veiling caused by the accretion disk in a consistent way. We have used a 2 minimization procedure to explore a grid of 800,000 LTE synthetic spectra computed for a plausible range of both stellar and veiling parameters. Adopting the best model parameters found, we have determined atmospheric abundances of Fe, Ca, Ti, Ni, and Al. The Fe abundance of the star is ½Fe=H ¼ 0:14 AE 0:20. Except for Ca, we found the other elements moderately overabundant as compared with stars in the solar neighborhood of similar iron content. Taking into account the small orbital separation, the mass transfer rate, and the mass of the convection zone of the secondary star, a comparison with element yields in supernova explosion models suggests a possible explosive event with a mass cut comparable to the current mass of the compact object. We have also analyzed the Li abundance, which is unusually high for a star of this spectral type and relatively low mass.

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The quiescent light curve and the evolutionary state of GRO J1655-40

Cited by 129 publications

References 38 publications

On the distance of GRO J1655-40

On the distance of GRO J1655-40

Compact Binary Merger Rates: Comparison With Ligo/Virgo Upper Limits

Chemical Abundances in the Secondary Star in the Black Hole Binary A0620−00

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