Exploring accretion disk physics and black hole growth with regular monitoring of ultrafast active galactic nucleus winds

Pounds, K. A.; Lobban, A.; Nixon, Chris

doi:10.1002/asna.201713338

Cited by 6 publications

(4 citation statements)

References 37 publications

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“…Most important is the fact that the observation of the AGN radiation variability is the result of the accretion rate variability in the SMBH at the center of its host galaxy. Among the most well-known scenarios of the basic structure of the accretion disk, which can explain the AGN strong and rapid variability, are the models of magnetically elevated (or "thick") disks (see (Dexter et al, 2014;Begelman et al, 2015;Begelman and Silk, 2017;Dexter and Begelman, 2018)), the transitions of the accretion state (see (Noda and Done, 2018;Ruan et al, 2019;Graham et al, 2019)), instability arising as a result of the magnetic moment near the inner stable circular orbit around the accretion disk (see (Stern et al, 2018;Ross et al, 2018)) and the misaligned disks (see (Nixon et al, 2012(Nixon et al, , 2013Nealon et al, 2015;Nixon and King, 2016;Pounds et al, 2017Pounds et al, , 2018King and Nixon, 2018)) and disk wind models (see (Elitzur and Shlosman, 2006;Elitzur and Ho, 2009;Elitzur et al, 2014;MacLeod et al, 2019)).…”

Section: Thermomagnetic Ettingshausen-nernst Effect Near Quantum Phas...mentioning

confidence: 99%

Thermomagnetic Ettingshausen-Nernst effect in tachocline, magnetic reconnection phenomenon in lower layers, axion mechanism of solar luminosity variations, coronal heating problem solution and mechanism of ADM variations around BH

Rusov,

Eingorn,

Sharph

et al. 2019

Preprint

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It is shown that the holographic principle of quantum gravity (in the hologram of the Universe, and therefore in our Galaxy, and of course on the Sun!), in which the conflict between the theory of gravitation and quantum mechanics disappears, gives rise to the Babcock-Leighton holographic mechanism. Unlike the solar dynamo models, it generates a strong toroidal magnetic field by means of the thermomagnetic Ettingshausen-Nernst (EN) effect in the tachocline. Hence, it can be shown that with the help of the thermomagnetic EN effect, a simple estimate of the magnetic pressure of an ideal gas in the tachocline of e.g. the Sun can indirectly prove that by using the holographic principle of quantum gravity, the repulsive toroidal magnetic field of the tachocline (B Sun tacho = 4.1 • 10 7 G = −B Sun core ) precisely "neutralizes" the magnetic field in the Sun core, since the projections of the magnetic fields in the tachocline and the core have equal values but opposite directions. The basic problem is a generalized problem of the antidynamo model of magnetic flux tubes (MFTs), where the nature of both holographic effects (the thermomagnetic EN effect and Babcock-Leighton holographic mechanism), including magnetic cycles, manifests itself in the modulation of asymmetric dark matter (WIMP ADM) and, consequently, the solar axion in the Sun interior.The general laws of the theory of virtually empty anchored flux tubes with B ∼ 10 7 G, which are born on the interface between the tachocline and the overshoot layer, are developed. These flux tubes are pushed out by means of the effective increase in their magnetic buoyancy -from the tachocline to the surface of the Sun. The appearance of MFTs on the surface of the Sun and the observed sunspots are identical. This means that the formation of the magnetic cycles of flux tubes coincides with the observational data of the Joy's Law, and both effects are the manifestation of dark matter (DM) -solar axions in the core of the Sun, the modulation of which is predetermined by the anticorrelation modulation of ADM.It is shown that the hypothesis of the axion mechanism of solar luminosity variations suggesting that the solar axion particles are born in the core of the Sun and may be efficiently

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Section: Thermomagnetic Ettingshausen-nernst Effect Near Quantum Phas...mentioning

confidence: 99%

Thermomagnetic Ettingshausen-Nernst effect in tachocline, magnetic reconnection phenomenon in lower layers, axion mechanism of solar luminosity variations, coronal heating problem solution and mechanism of ADM variations around BH

Rusov,

Eingorn,

Sharph

et al. 2019

Preprint

View full text Add to dashboard Cite

show abstract

“…As an example, in Figure we show a portion of an RGS spectrum of the Seyfert galaxy PG1211+143, from the work of Pounds et al (, ) (see also Pounds et al , in this volume). Based on both prior EPIC‐PN studies (Pounds et al ) and the more recent RGS studies, it has been argued that PG1211+143 exhibits blueshifted, ionized outflows moving at speeds in the galaxy rest frame of

scriptO ((), 10 %)

the speed of light.…”

Section: Xmm‐newton/chandra Synergiesmentioning

confidence: 99%

Leveraging high‐resolution spectra to understand black hole spectra

Nowak

2017

Astron Nachr

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For the past 17 years, both XMM-Newton and Chandra have brought the powerful combination of high spatial and spectral resolution to the study of black hole systems. Each of these attributes requires special consideration-in comparison to lower spatial resolution charge-coupled device (CCD)-quality spectra-when modeling observations obtained by these spacecraft. A good understanding of the high-resolution spectra is in fact required to model properly lower resolution CCD spectra, with the reflection grating spectrometer (RGS) instrument on XMM-Newton maintaining the highest "figure of merit" at soft X-ray energies for all missions flying or currently planned for the next decade. Thanks to its even higher spectral resolution, the use of Chandra high-energy transmission gratings (HETGs), albeit with longer integration times, allows for one to bring further clarity to RGS studies. A further promising route for continued studies is the combination of high spectral resolution at soft X-rays, via RGS and/or HETG, with contemporaneous broadband coverage extending to hard X-rays (e.g., NuSTAR or INTEGRAL spectra). Such studies offer special promise for answering fundamental questions about accretion in black hole systems; however, they have received only moderate consideration to date. This may be due in part to the difficulty of analyzing high-resolution spectra. In response, we must continue to develop software tools that make the analysis of high-resolution X-ray spectra more accessible to the wider astrophysics community.

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“…Considering the simultaneous observation of multiple ex-panding shells of absorbing gas in the context of super-Eddington accretion, Pounds, Lobban and Nixon (2017) noted that short-lived wind components might be a natural consequence of the way in which matter accretes in an AGN, typically falling from far outside the sphere of gravitational influence of the SMBH and with essentially random orientation. The resulting accretion stream will in general orbit in a plane misaligned to the spin of the central black hole (King & Pringle 2006, 2007, with the inner disc subject to Lense-Thirring precession around the spin vector, and orbits at smaller radii precessing sufficiently fast to cause the tearing-away of independent rings of gas.…”

Section: Introductionmentioning

confidence: 99%

Are ultrafast inflows in AGN truly rare -- or just much harder to see?

Pounds¹

2022

Preprint

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Short-term variability and multiple velocity components in the powerful highly ionized wind of the archetypal UFO PG1211+143 are indicative of inner disc instabilities or short-lived accretion events. The detection of a high velocity (∼ 0.3c) inflow of highly ionized matter, located at 20 R g , offered the first direct observational support for the latter scenario, where matter approaching at a high inclination to the black hole spin plane may result in warping and tearing of the inner accretion disc, with subsequent inter-ring collisions producing shocks, loss of rotational support and rapid mass infall. Simultaneous soft x-ray spectra reveal a lower velocity (∼ 0.1c) inflow of less ionized matter, identified as 'upstream' at 200 R g , with a line of sight through matter converging on the supermassive black hole. We discuss here why ultrafast ionized winds are relatively common in luminous Seyfert galaxies, while detection of the 0.3c inflow in PG1211+143 remains a rare example.

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Exploring accretion disk physics and black hole growth with regular monitoring of ultrafast active galactic nucleus winds

Cited by 6 publications

References 37 publications

Thermomagnetic Ettingshausen-Nernst effect in tachocline, magnetic reconnection phenomenon in lower layers, axion mechanism of solar luminosity variations, coronal heating problem solution and mechanism of ADM variations around BH

Thermomagnetic Ettingshausen-Nernst effect in tachocline, magnetic reconnection phenomenon in lower layers, axion mechanism of solar luminosity variations, coronal heating problem solution and mechanism of ADM variations around BH

Leveraging high‐resolution spectra to understand black hole spectra

Are ultrafast inflows in AGN truly rare -- or just much harder to see?

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