Radio Emission from GRO J1655−40 during the 1994 Jet Ejection Episodes

Hannikainen, D. C.; Hunstead, R. W.; Campbell-Wilson, D.; Wu, Kinwah; McKay, D. J.; Smits, Derck P.; Sault, R. J.

doi:10.1086/309294

Cited by 50 publications

(81 citation statements)

References 19 publications

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“…After TJD 9589 the circular polarization is consistent with zero, with measured values between 0.6 ± 1.0 mJy and −0.3 ± 2.0 mJy at 4.8 GHz and between −0.7 ± 1.5 and −0.5 ± 1.5 mJy at 8.6 GHz. Figure 1 shows that several large changes in the 1.4 and 2.4 GHz circular polarization lightcurves bear a close resemblance to the flares identified in the linear polarization by Hannikainen et al (2000), as marked. For instance, the rise and decay of the first circularly polarized outburst shows a corresponding burst in the linear polarization over the same epoch, from TJD 9580-9583.…”

Section: Resultsmentioning

confidence: 64%

“…The circular polarization observed is the sum of the contributions from all previous ejections. Hannikainen et al (2000) identify three separate ejection events in the period TJD 9579-9598 on the basis of the linearly polarized emission detected by ATCA at TJDs ∼9582, 9587 and 9591.…”

Section: Circular Polarization Variationsmentioning

confidence: 94%

“…2. The linear polarization plots are adopted from Hannikainen et al (2000), and the errors in these curves are ∼1 mJy. b) Lightcurves of the variations in Stokes I at the same four frequencies.…”

Section: Data Reductionmentioning

confidence: 99%

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Rapidly evolving circularly polarized emission during the 1994 outburst of GRO J1655–40

Macquart

Sault

et al. 2002

A&A

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Abstract. We report the detection of circular polarization during the 1994 outburst of the Galactic microquasar GRO J1655−40. The circular polarization is clearly detected at 1.4 and 2.4 GHz, but not at 4.8 and 8.4 GHz, where its magnitude never exceeds 5 mJy. Both the sign and magnitude of the circular polarization evolve during the outburst. The time dependence and magnitude of the polarized emission can be qualitatively explained by a model based on synchrotron emission from the outbursts, but is most consistent with circular polarization arising from propagation effects through the relativistic plasma surrounding the object.

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Section: Resultsmentioning

confidence: 64%

Section: Circular Polarization Variationsmentioning

confidence: 94%

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Rapidly evolving circularly polarized emission during the 1994 outburst of GRO J1655–40

Macquart

Sault

et al. 2002

A&A

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“…The flat-top profile is inconsistent with a single expanding bubble emitting synchrotron radiation, but can be explained by a jet or a series of successive bubbles. The very short duration of the echo outburst resembles the radio flares observed during the X-ray outburst of the microquasar GRO J1655-40 [3].…”

Section: Resultsmentioning

confidence: 61%

Long-term optical activity of the microquasar V4641 Sgr

Šimon¹,

Henden²

2009

Proceedings of VII Microquasar Workshop: Microquasars and Beyond — PoS(MQW7)

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We present an analysis of the optical activity of the microquasar V4641 Sgr using the visual and photographic data. We analyze four smaller (echo) outbursts that followed the main outburst (1999). Their mean recurrence time T C is 377 days, with a trend of a decrease. We interpret the characteristic features of the recent activity of V4641 Sgr (the narrow outbursts separated by a long quiescence, a clear trend in the evolution of their T C ) as the thermal instability of the accretion disk operating in dwarf novae and soft X-ray transients. We argue that the luminosity of four echo outbursts is too high to be explained by the thermal emission of the accretion disk. We interpret them as due to the thermal instability, in which the outburst gives rise to a jet radiating also in the optical. This supports the finding by Uemura et al., PASJ 54, L79 (2002). The pre-outburst observations (1964)(1965)(1966)(1967) reveal ongoing activity of the system. It displays low-amplitude fluctuations on the timescale of several weeks, independent on the orbital phase. In addition, a larger brightening which lasted for several tens of days and occurred from the level of brightness higher than in other years can be resolved.

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“…The only evidence of ordered magnetic fields in LMXBs jets has been observed for the persistent system Cyg X-1 (Russell & Shahbaz 2014). Only a few LMXBs have been observed with polarimetric techniques to date, both persistent and transient ones (Charles et al 1980;Dolan & Tapia 1989;Gliozzi et al 1998;Hannikainen et al 2000;Schultz et al 2004;Brocksopp et al 2007;Shahbaz et al 2008a;Russell & Fender 2008;Russell et al 2011;Baglio et al 2014).…”

Section: Polarimetric Signatures Of a Jetmentioning

confidence: 99%

Polarimetric and spectroscopic optical observations of the ultra-compact X-ray binary 4U 0614+091

Baglio

Mainetti

D’Avanzo

et al. 2014

A&A

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Aims. We present a polarimetric and spectroscopic study of the persistent ultra-compact X-ray binary 4U 0614+091 aimed at searching for the emission of a relativistic particle jet and at unveiling the orbital period P orb of the system. Methods. We obtained r-band polarimetric observations with the Telescopio Nazionale Galileo (TNG) equipped with the PAOLO polarimeter and with the Nordic Optical Telescope (NOT) equipped with the ALFOSC instrument, covering ∼2 h and ∼0.5 h observations, respectively. We carried out low resolution spectroscopy of the system using the ESO Very Large Telescope equipped with FORS1 for ∼1.5 h (16 spectra covering the range 4300−8000 Å).Results. The polarimetric analysis performed starting from the TNG dataset revealed a polarisation degree in the r-band of 3% ± 1%. From the NOT dataset, due to the lower signal-to-noise ratio, we could obtain only a 3σ upper limit of 3.4%. From the joining of a spectroscopic and photometric analysis, through the study of the equivalent width variations of the CII 7240 Å line and the r-band light curve, we could find a hint of a ∼45 min periodicity. Conclusions. A polarisation degree P of ∼3% in the r-band is consistent with the emission of a relativistic particle jet, which is supposed to emit intrinsically linearly polarised synchrotron radiation. Since no variations of P with time have been detected, and the accretion disc of the system does not contain ionised hydrogen, scattering by free electrons in the accretion disc has been rejected. The period of ∼45 min obtained through the analysis of the system light curve and of the equivalent width variations of the selected spectral line is probably linked to the presence of a hot spot or a superhump in the accretion disc, and lead to an orbital period 1 h for the binary system.

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Radio Emission from GRO J1655−40 during the 1994 Jet Ejection Episodes

Cited by 50 publications

References 19 publications

Rapidly evolving circularly polarized emission during the 1994 outburst of GRO J1655–40

Rapidly evolving circularly polarized emission during the 1994 outburst of GRO J1655–40

Long-term optical activity of the microquasar V4641 Sgr

Polarimetric and spectroscopic optical observations of the ultra-compact X-ray binary 4U 0614+091

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