Indisputable evidence for supermassive black hole binary systems in AGN| Urania

The study of blasari flux variability focuses on analyzing the precession, which is caused by the presence of black holes spinning at the centers of galaxies.

An international research team led by Silke Pritzen of the Max Planck Institute for Radio Astronomy in Bonn conducted a search for this planet. BlazersAccumulation supermassive black holes in the centers galaxies. Blazars spawn when nobody is streams emitted from active galactic nucleus It is directed directly towards the Earth. Scientists provide evidence that the variability observed in blazars is a consequence The initiative The source of the outflow, which could be caused by the presence of a second supermassive black hole near the primary black hole or by a tortuous accumulator disc around a single black hole.

Over decades of blazar observations, the results have always been interpreted to mean that frequent and large bursts of brightness from these sources, called flare activity, are associated with the ejection of flow components from the core into the jets. This phenomenon leads to a sudden increase in emissions.

Blizzard planes often exhibit twisted shapes that are not as straight as one might expect. These tortuous flow structures were initially thought to be associated with the ejection of components from the core. The tortuous flows and brightness of the active galactic nucleus (AGN) are thought to be caused by the random feeding of the black hole. However, over the years, increasingly detailed observations have called into question this possibly very simple causal relationship.

New article published In The Astrophysical Journal, he challenges the relationship between ejecta and glow in bright, highly variable blazers. Lead author of the study Silke Pritzen presents the evidence and discusses the possibility that motion of the jet source, caused either by a supermassive black hole in a binary at the foot of the jet, or, more likely, by an accretion disk twisted around a single black hole, is responsible for the observed fluctuations.

When the streams rotate due to prior motion, this eddy motion naturally leads to periodic changes, also in intensity, due to Doppler effect. This effect has been detected in AGN streams over many years.

In the case of OJ 287, which is considered the best candidate for a supermassive black hole in a binary system, Silk-Pritzen and her team determined that strong changes in the brightness and curvature of the jet are antecedent in origin, as they show in their Rosetta paper. Recently, predictions from their work have been confirmed by Comosa and other scientists.

The research team has now applied the same model to other analyzes. By examining a sample of 12 AGNs, their results show that the difference in brightness and curvature of the jets can indeed be explained by modulation due to precession.

The authors do not deny that the physics of the flow can be caused by internal interactions in the flow, which the flow shock model explains, and instabilities in the flow beam. However, they suggest that the appearance of these jets is strongly modulated and changed by the movement of the jets. According to their suggestion, these streams would not be so curved and bright if they were not enhanced by the precession effect.

By unleashing the relationship between brightness enhancement and flux component expulsion, the interaction between the dynamical system can be studied, which is fundamentally predictable because it can be interpreted in an engineering context.

The diversity of blazars in many galaxies may not be random, but rather inevitable Silk-Britzen said. It is interesting to decipher the inner workings of this black hole mechanism by studying the fluctuations.

One of the main findings of this study is that the curvature of the jets may be an important indicator of the presence of binary black holes at the centers of these galaxies. It appears that the stream is forced to meander by the effect of the second black hole’s gravity on the black hole from which this stream is emitting. In addition, the research team was able to detect traces Gesture movement With a smaller amplitude in both radios slight curvesAs well as in the kinetics of the components of the stream.

The physics of accretionary disks and jets is very complex, but their kinematics can be compared to simple gyroscopes. If the accretion disk is subjected to an external torque, such as that produced by a spinning black hole, the disk will precess the nod, similar to Earth’s axis of rotation, which is affected by the moon and sun – explains Michal Zagacek of Masaryk University (Brno, Czech Republic), one of the authors of this study.

Radio observations achieve the highest precision in astronomical observations by combining radio telescopes at very long distances using long fundamental interferometry Very Long Baseline Radio Interferometry (VLBI). This is the same method that allowed the team Event Horizon Telescope (EHT) The shadow of a black hole was detected for the first time by observing a black hole with a mass of 6.5 billion solar masses Galaxy M87.

The search for these close pairs of supermassive black holes has been going on for decades, and it’s like looking for a needle in a haystack.

At the moment, we still lack sufficient precision to directly study the existence of binary supermassive black holes. However, the flow initiative appears to be the most promising signature for these objects. This discovery is welcomed not only by the scientific community of the black hole and active galaxies, but also by the research community gravitational waves I pulsars. Evidence for the cosmic background of gravitational waves originating from mergers of massive black holes has recently been published in cosmic history Silk-Pritzen concluded.

Details:
Agnes Nowak

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Credit: Max Planck Institute for Radio Astronomy

Pictured: The image shows a magnetized radio flux (yellow) moving under the influence of the supermassive black hole at the center of the galaxy. The image shows a supermassive black hole, shown in black, at the center of the accretion disk. This disk contains warmer gas (blue) and cooler gas (red). The white arrow points in the direction of rotation of the larger black hole. The second black hole (orange) orbits the central supermassive black hole, and the orange arrow shows the direction of the orbital angular momentum. Source: Michal Zagaczyk/UTFA MUNI