The X-ray transient XTE J1859 + 226 in outburst and quiescence

Zurita, C.; Sánchez–Fernández, C.; Casares, J.; Charles, P. A.; Abbott, T. M. C.; Hakala, Pasi; Rodríguez‐Gil, P.; Bernabei, S.; Piccioni, A.; Гуарниери, А.; Bartolini, C.; Masetti, N.; Shahbaz, T.; Castro-Tirado, A. J.; Henden, A. A.

doi:10.1046/j.1365-8711.2002.05588.x

Cited by 60 publications

(77 citation statements)

References 35 publications

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“…A follow-up observation of the source with the RXTE/PCA (Proportional Counter Array, 2−60 keV) revealed a hard power-law dominated spectrum (Markwardt et al 1999). On October 16, the source reached its peak flux of ∼5 × 10 −8 erg s −1 cm −2 in the 2−80 keV band (corresponding to a luminosity of ∼7 × 10 38 erg s −1 for an assumed distance of 11 kpc (Zurita et al 2002)). After the initial hard rise, XTE J1859+226 softened at its peak intensity and continued to soften for almost two months, when a secondary hard plateau took place (see Fig.…”

Section: Sobczak Et Al 2000)mentioning

confidence: 99%

A study of the low-frequency quasi-periodic oscillations in the X-ray light curves of the black hole candidate XTE J1859+226

Casella

Belloni

Homan

et al. 2004

A&A

216

319

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Abstract. We present the results of an extensive timing analysis of the 1999 outburst of the soft X-ray transient and black hole candidate XTE J1859+226 as observed with the Rossi X-Ray Timing Explorer. Three main different types of low frequency (1−9 Hz) quasi-periodic oscillations (QPOs) were observed and classified, strengthening the general picture that is emerging for the variability properties of black hole X-ray binaires. Rapid transitions between different power spectral shapes were observed and their link with the count rate was studied. Furthermore, we show that a frequency of ∼6 Hz seems to hold a particular place: one of the three QPO types we found was very stable when at this frequency, as it happens in Z sources as well. The coherence of its subharmonic peak was higher when the fundamental was close to 6 Hz, thus suggesting the presence of some resonance at this frequency.

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Section: Sobczak Et Al 2000)mentioning

confidence: 99%

A study of the low-frequency quasi-periodic oscillations in the X-ray light curves of the black hole candidate XTE J1859+226

Casella

Belloni

Homan

et al. 2004

A&A

216

319

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“…The positions are taken from 2MASS, and the distances, orbital periods, and mass function are from McClintock & Remillard (2006). For the remaining data, the references are as follows: (1) A0620Ϫ00: Gelino et al (2001) for all photometry and the spectral type; (2) GS 2023ϩ338: Casares et al (1993) for all photometry and the spectral type; (3) XTE J1118ϩ480: spectral type from Torres et al (2004), extinction from McClintock et al (2003), J and K from Mikołajewsa et al (2005), B from USNO, and R from Zurita et al (2002); (4) Cen X-4: spectral type from Shahbaz et al (1993) and Torres et al (2002), J, H, and K from 2MASS; other bands from Shahbaz et al (1993).…”

Section: Observations and Data Analysismentioning

confidence: 99%

Mid-Infrared Emission from Dust around Quiescent Low-Mass X-Ray Binaries

Muno

Mauerhan

2006

ApJ

113

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We report the discovery of excess 4.5 and 8 mm emission from three quiescent black hole low-mass X-ray binaries, A0620Ϫ00, GS 2023ϩ338, and XTE J1118ϩ480, and the lack of similar excess emission from Cen X-4. The mid-infrared emission from GS 2023ϩ338 probably originates in the accretion disk. However, the excess emission from A0620Ϫ00 and XTE J1118ϩ480 is brighter and peaks at longer wavelengths, and thus most likely originates from circumbinary dust that is heated by the light of the secondary star. For these two sources, we find that the inner edges of the dust distributions lie near 1.7 times the binary separations, which are the minimum radii at which circumbinary disks would be stable against tidal disruption. The excesses are weak at 24 mm, which implies that the dust does not extend beyond about 3 times the binary separations. The total masses of circumbinary material are between and g. The material could be the remains of fallback 22 24 10 10 disks produced in supernovae, or material from the companions injected into circumbinary orbits during mass transfer.

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“…b Updated after Casares et al (2007). c Period is uncertain, with another possibility at 0.319 days (see Zurita et al 2002). This would drop the mass function to 6.18 M⊙.…”

Section: From "Candidates" To Confirmed Bhsmentioning

confidence: 99%

Observational evidence for stellar-mass black holes

Casares

2006

Proc. IAU

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Abstract. Radial velocity studies of X-ray binaries provide the most solid evidence for the existence of stellar-mass black holes. We currently have 20 confirmed cases, with dynamical masses in excess of 3 M⊙. Accurate masses have been obtained for a subset of systems which gives us a hint at the mass spectrum of the black hole population. This review summarizes the history of black hole discoveries and presents the latest results in the field.

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The X-ray transient XTE J1859 + 226 in outburst and quiescence

Cited by 60 publications

References 35 publications

A study of the low-frequency quasi-periodic oscillations in the X-ray light curves of the black hole candidate XTE J1859+226

A study of the low-frequency quasi-periodic oscillations in the X-ray light curves of the black hole candidate XTE J1859+226

Mid-Infrared Emission from Dust around Quiescent Low-Mass X-Ray Binaries

Observational evidence for stellar-mass black holes

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