A Transient Radio Jet in an Erupting Dwarf Nova

Körding, Elmar; Rupen, M. P.; Knigge, Christian; Fender, R. P.; Dhawan, V.; Templeton, Matthew R.; Muxlow, T. W. B.

doi:10.1126/science.1155492

Cited by 150 publications

(226 citation statements)

References 25 publications

Supporting

Mentioning

202

Contrasting

Order By: Relevance

“…Such comparisons could be problematic because LX does not provide a good estimate for Pacc in supermassive BHs as it does for XRBs (Pellegrini 2005). Nevertheless, Merloni & Heinz (2007) and Körding et al (2008) both found the estimates of the scaled jet power compared to the accretion power for Cygnus X-1 to be consistent with those of their AGN samples, albeit with large uncertainties comparable to the uncertainties in the jet power that we find in this work. In contrast, King et al (2013) claimed to find a discrepancy between the jet and wind-scaling correlations with the bolometric luminosity and the values found for Cygnus X-1 using different scaling relations.…”

Section: The Black Hole Jetsupporting

confidence: 67%

Shell-shocked: the interstellar medium near Cygnus X-1

Sell

Heinz

Richards

et al. 2014

Monthly Notices of the Royal Astronomical Society

View full text Add to dashboard Cite

We conduct a detailed case-study of the interstellar shell near the high-mass X-ray binary, Cygnus X-1. We present new WIYN optical spectroscopic and Chandra X-ray observations of this region, which we compare with detailed MAPPINGS III shock models, to investigate the outflow powering the shell. Our analysis places improved, physically motivated constraints on the nature of the shockwave and the interstellar medium (ISM) it is plowing through. We find that the shock is traveling at less than a few hundred km s −1 through a low-density ISM (< 5 cm −3 ). We calculate a robust, 3σ upper limit to the total, time-averaged power needed to drive the shockwave and inflate the bubble, < 2×10 38 erg s −1 . We then review possible origins of the shockwave. We find that a supernova origin to the shockwave is unlikely and that the black hole jet and/or O-star wind can both be central drivers of the shockwave. We conclude that the source of the Cygnus X-1 shockwave is far from solved.

show abstract

Section: The Black Hole Jetsupporting

confidence: 67%

Shell-shocked: the interstellar medium near Cygnus X-1

Sell

Heinz

Richards

et al. 2014

Monthly Notices of the Royal Astronomical Society

View full text Add to dashboard Cite

show abstract

“…For all but the last, their velocities are (at least mildy) relativistic (Reipurth & Bally 2001;Körding et al 2008a;Mirabel & Rodríguez 1999). Despite a wealth of observations, the launch mechanism of jets has so far remained elusive.…”

Section: Introductionmentioning

confidence: 99%

The contribution of spin to jet-disk coupling in black holes

Velzen

Falcke

2013

A&A

View full text Add to dashboard Cite

Context. The spin of supermassive black holes could power jets from active galactic nuclei (AGN), although direct observational evidence for this conjecture is sparse. The accretion disk luminosity and jet power, on the other hand, have long been observed to follow a linear correlation. Aims. If jet power is coupled to black hole spin, deviations from the jet-disk correlation for a sample of AGN can be used to probe the dispersion of the spin parameter (a) within this sample. Methods. To obtain a large sample of radio-loud AGN, we matched double-lobed radio sources identified in Faint Images of the Radio Sky at Twenty-centimeters (FIRST, 1.4 GHz) to spectroscopically confirmed quasars from the Sloan Digital Sky Survey (SDSS). We obtain 763 FR II quasars with a median redshift of z = 1.2. Results. A tight correlation between the optical luminosity of the accretion disk and the lobe radio luminosity is observed. We estimate that 5-20% of the bolometric disk luminosity is converted to jet power. Most of the scatter to the optical-radio correlation is due to environment; deviations from jet-disk coupling due to internal factors (e.g., spin) contribute at most 0.2 dex. Conclusions. Under the assumption that the Blandford-Znajek mechanism operates in AGN, we obtain an upper limit of 0.1 dex to the dispersion of the product of the spin and the magnetic flux threading the horizon. If black hole spin determines the AGN jet efficiency, then our observations imply that all FR II quasars have very similar spin. In addition, the quasar spin distribution needs to have a wide gap to explain the radio-quiet population. The alternative, and perhaps more likely, interpretation of the tight jet-disk correlation is that black hole spin is not relevant for powering AGN jets.

show abstract

“…Kording et al 2006;Kording et al 2008;Tudose et al 2009), argues for an ejection process that is also independent of the central object. This seems to be confirmed by the lack of correlation between jet power or jet velocities and measured values of black hole spins (Fender et al 2010).…”

Section: Introductionmentioning

confidence: 99%

Relevance of jet emitting disc physics to microquasars: application to Cygnus X-1

Petrucci

Ferreira

Henri

et al. 2010

A&A

View full text Add to dashboard Cite

Context. Interpretation of the X-ray spectra of X-ray binaries during their hard states requires a hot, optically thin medium. There are several accretion disc models that account for this aspect. However, none is designed to simultaneously explain powerful jets detected during these states. Aims. A new quasi-Keplerian hot accretion disc solution, a jet emitting disc (JED hereafter), which is part of a global disc-jet MHD structure producing stationary super-alfvénic ejection, is investigated here. Its radiative and energetic properties are then compared to the observational constraints found in Cygnus X-1. Methods. We solve the disc energy equation by balancing the local heating term with advection and cooling by synchrotron, bremsstrahlung, and Comptonization processes. The heating term, disc density, accretion velocity, and magnetic field amplitude were taken from published self-similar models of accretion-ejection structures. Both optically thin and thick regimes are considered in a one-temperature, gas-supported disc. Results. Three branches of solutions are found to be possible at a given radius, but we only investigate the hot, optically thin and geometrically slim solutions. These solutions give simultaneously and consistently the radiative and energetics properties of the discjet system. They are able to reproduce the global accretion-ejection properties of Cygnus X-1 very well, namely its X-ray spectral emission, jet power, and jet velocity. About half of the released accretion power is used to produce two mildly relativistic (v/c 0.5) jets, and for a luminosity of about 1% of the Eddington luminosity, the JED temperature and optical depth are close to what is observed in the hard state of Cygnus X-1. Conclusions. The accretion and ejection properties of JEDs agree with the observations of the prototypical black hole binary Cygnus X-1. The JED solutions are likely to be relevant to the whole class of microquasars.

show abstract

A Transient Radio Jet in an Erupting Dwarf Nova

Cited by 150 publications

References 25 publications

Shell-shocked: the interstellar medium near Cygnus X-1

Shell-shocked: the interstellar medium near Cygnus X-1

The contribution of spin to jet-disk coupling in black holes

Relevance of jet emitting disc physics to microquasars: application to Cygnus X-1

Contact Info

Product

Resources

About