Accretion of dissipative dark matter onto active galactic nuclei

Outmezguine, Nadav Joseph; Slone, Oren; Tangarife, Walter; Ubaldi, Lorenzo; Volansky, Tomer

doi:10.1007/jhep11(2018)005

Cited by 11 publications

(7 citation statements)

References 193 publications

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“…We focus on the "mild cooling regime", in which the cooling timescale is longer than the free-fall time of the halo. In this case, the halo mostly stays in hydrostatic equilibrium and contracts as a whole without fragmentation, as opposed to situations with strong cooling [36][37][38][39].…”

Section: Imentioning

confidence: 99%

Constraining Dissipative Dark Matter Self-Interactions

et al. 2019

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We study the gravothermal evolution of dark matter halos in the presence of dissipative dark matter self-interactions. Dissipative interactions are present in many particle-physics realizations of the dark-sector paradigm and can significantly accelerate the gravothermal collapse of halos compared to purely elastic dark matter self-interactions. This is the case even when the dissipative interaction timescale is longer than the free-fall time of the halo. Using a semi-analytical fluid model calibrated with isolated and cosmological N -body simulations, we calculate the evolution of the halo properties -including its density profile and velocity dispersion profile -as well as the core-collapse time as a function of the particle model parameters that describe the interactions. A key property is that the inner density profile at late times becomes cuspy again. Using 21 dwarf galaxies that exhibit a core-like dark matter density profile, we derive constraints on the strength of the dissipative interactions and the energy loss per collision.

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Section: Imentioning

confidence: 99%

Constraining Dissipative Dark Matter Self-Interactions

et al. 2019

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“…• The most important point is the fact that "understanding the relationship between the galaxies in which the active galactic nuclei (AGNs) are located and the halo of dark matter in which they are located is the key to limiting how black hole refueling is triggered and regulated" (Leauthaud et al, 2015;Netzer, 2013;Gatti et al, 2016;Ballantyne, 2017;Padovani et al, 2017;Georgakakis et al, 2018;Outmezguine et al, 2018).…”

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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“…This accretion rate could be affected by the dissipative interactions, an effect which we do not consider here but which has been explored in[54].…”

mentioning

confidence: 99%

Early formation of supermassive black holes via dark matter self-interactions

Choquette

Cline

Cornell

2019

J. Cosmol. Astropart. Phys.

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The existence of supermassive black holes at high redshifts (z ∼ 7) is difficult to accommodate in standard astrophysical scenarios. It has been shown that dark matter models with a subdominant self-interacting component are able to produce early seeds for supermassive black holes through the gravothermal catastrophe. Previous studies used a fluid equation approach, requiring some limiting assumptions. Here we reconsider the problem using N -body gravitational simulations starting from the formation of the initial dark matter halo. We consider both elastic and dissipative scattering, and elucidate the interplay between the dark matter microphysics and subsequent accretion of the black hole needed to match the properties of observed high redshift supermassive black holes. We find a region of parameter space in which a small component of self-interacting dark matter can produce the observed high redshift supermassive black holes.

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Accretion of dissipative dark matter onto active galactic nuclei

Cited by 11 publications

References 193 publications

Constraining Dissipative Dark Matter Self-Interactions

Constraining Dissipative Dark Matter Self-Interactions

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

Early formation of supermassive black holes via dark matter self-interactions

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