Correlations between X-ray outbursts and relativistic ejections in the X-ray transient GRO J1655 – 40

Harmon, B. A.; Wilson, C. A.; Zhang, S. N.; Pačiesas, W. S.; Fishman, G. J.; Hjellming, R. M.; Rupen, M. P.; Scott, D. M.; Briggs, M. S.; Rubin, B. C.

doi:10.1038/374703a0

Cited by 123 publications

(103 citation statements)

References 6 publications

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“…The authors build a kinematic model of the radio jets of GRO J1655-40 and obtain a distance of 3.2 ± 0.2 kpc. The authors do not actually measure the distance directly, but refer to McKay & Kesteven (1994), Tingay et al (1995) and Harmon et al (1995). Their model provides a refinement of the distance range obtained by the cited authors.…”

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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“…Outbursts in microquasars are characterised by an X-ray outburst close to periastron followed by the formation of a radio jet at a later time, when the X-ray spectrum indicates that the inner part of the accretion disc has vanished (Harmon et al 1995). The Kreykenbohm et al 2004;c White et al 1976. radio outburst can therefore be delayed by up to some 10 days relative to the X-ray outburst.…”

Section: Introductionmentioning

confidence: 99%

Radio emission from the high-mass X-ray binary BP Crucis

Pestalozzi

Torkelsson

Hobbs

et al. 2009

A&A

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Context. BP Cru is a well known high-mass X-ray binary consisting of a late B hypergiant (Wray 977) and a neutron star, also observed as the X-ray pulsar GX301-2. No information about emission from BP Cru in bands other than X-rays and optical has been reported. A massive X-ray binaries containing black holes can produce radio emission from a jet. Aims. To assess the presence of a radio jet, we searched for radio emission from BP Cru using the Australia Compact Array Telescope as part of a survey for radio emission from Be/X-ray transients. Methods. We probed the 41.5 d orbit of BP Cru with the Australia Telescope Compact Array, close to both periastron and apastron. Results. BP Cru was clearly detected in our data on 4, possibly 6, of 12 occasions at 4.8 and 8.6 GHz. Our data suggest that the spectral index of the radio emission is modulated either by the X-ray flux or the orbital phase of the system. Conclusions. We propose that the radio emission of BP Cru probably originates in two components: a persistent component, related to the mass donor Wray 977, and a periodic component, connected to accretion onto the neutron star, possibly originating from a (weak and short lived) jet.

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“…It is one of only six Galactic superluminal sources observed so far, the others being 1E1740·7-2942 , GRS 1758-258 (Rodriguez, Mirabel & Marti 1992), GRS 1915+105 (Mirabel & Rodriguez 1994), XTE J1819-284 (Hjellming et al 1999) and XTE J1748-288 (Hjellming et al 1998). This lowmass X-ray binary (LMXB) has been extensively studied at most wavelengths (Harmon et al 1995;Kroeger et al 1996;Tavani et al 1996;Hynes et al 1998a,b). Due to its distance of only 3·2 ± 0·2 kpc (Hjellming & Rupen 1995) and relatively large quiescent brightness compared to those of other LMXBs (V = 17·3 mag; Bailyn et al 1995a), we have been able to study the companion star in this system with unprecedented coverage and accuracy.…”

Section: Introductionmentioning

confidence: 99%

Atmospheric Modelling of the Companion Star in GRO J1655-40

Buxton

Vennes

2001

Publ. – Astron. Soc. Aust

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We have measured the rotational velocity of the companion star to be Ʊrot sin i= 80 ± 10 km s ˗1 (1σ) by fitting Kurucz model spectra to our observed spectrum of the black-hole candidate GRO J1655–40. From this we have calculated q = 0·31 ± 0·08, the mass of the compact object to be M1 = 7·91 ± 3·79 Mô (1σ) and for the companion starM2 = 2·76 ± 1·79 Mô (1σ), which is consistent with previous studies. We have also determined Teff = 6500 ± 50 K and [Fe/H] = −0·15 +0·15-0·10.

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Correlations between X-ray outbursts and relativistic ejections in the X-ray transient GRO J1655 – 40

Abstract: LO 0)I'-I 0 _,,,.

Cited by 123 publications

References 6 publications

On the distance of GRO J1655-40

On the distance of GRO J1655-40

Radio emission from the high-mass X-ray binary BP Crucis

Atmospheric Modelling of the Companion Star in GRO J1655-40

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