Magnetic fields in galaxy clusters

Brüggen, M.

doi:10.1002/asna.201311895

Cited by 10 publications

(9 citation statements)

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“…Similar observations have allowed one to detect magnetic fields in larger structures, namely in clusters of galaxies (for reviews, see Carilli & Taylor, 2002;Govoni & Feretti, 2004;Feretti et al, 2012;Brüggen, 2013). Microgauss fields have thus been measured which, in most cases, are rather turbulent on scales ranging from a few hundreds of parsecs up to tens of kiloparsecs (Feretti et al, 2012).…”

Section: Magnetic Fields In the Universementioning

confidence: 89%

Baryonic Processes in the Large-Scale Structuring of the Universe

Durrive

2017

Springer Theses

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Section: Magnetic Fields In the Universementioning

confidence: 89%

Baryonic Processes in the Large-Scale Structuring of the Universe

Durrive

2017

Springer Theses

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“…Behaviour of concentration of different forms of hydrogen, which mostly was ionized, and molecular hydrogen was a several thousandth of a percent (see fig. 7), was modeled with using of code ChemPAK (Chernykh et al 2009) for specific values of temperature T = 1000 K and T = 5000 K, and also for specific concentration of atomic neutral hydrogen. In numerical experiment concentrations behaved in a similar way.…”

Section: Ei Recombination On Grains (Weingartner and Draine 2001)mentioning

confidence: 99%

“…Magnetic field plays a key role in formation and dynamics of astrophysical objects. Thus, on cosmological scales the influence of weak magnetic field, with order µG, on the dynamics of hydrodynamical instabilities and ram-pressure mechanism in galactic clusters (Bruggen 2013) was studied; primarily radial orientation of the magnetic field in Virgo cluster outside the central area was defined (Pfrommer & Dursi 2010), and comparison of magnetic field with radio observation was carried out (Xu et al 2012). The structure of magnetic field in spiral arms of the M51 galaxy was investigated (Fletcher et al 2011), and the evolution of the disk galaxy with consideration of influence of magnetic field was modeled (Pakmor & Springel 2013).…”

Section: Introductionmentioning

confidence: 99%

The numerical modelling of MHD astrophysical flows with chemistry

Kulikov

Chernykh

Protasov

2017

J. Phys.: Conf. Ser.

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The new code for numerical simulation of magnetic hydrodynamical astrophysical flows with consideration of chemical reactions is given in the paper. At the heart of the code -the new original low-dissipation numerical method based on a combination of operator splitting approach and piecewise-parabolic method on the local stencil. The details of the numerical method are described; the main tests and the scheme of parallel implementation are shown. The chemodynamics of the hydrogen while the turbulent formation of molecular clouds is modeled.

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“…In the case of the eddy-viscosity closure, τ * ij causes a diffusion effect on top of the numerical diffusion, which occurs regardless of the compressibility of the flow. 13 For strongly diffusive numerical schemes, this effect is marginal. For high-resolution schemes, on the other hand, the explicit turbulent stresses in LES can become significant.…”

Section: The Compressible Subgrid-scale Turbulence Energy Modelmentioning

confidence: 99%

Large Eddy Simulations in Astrophysics

Schmidt

2015

Living Rev Comput Astrophys

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In this review, the methodology of large eddy simulations (LES) is introduced and applications in astrophysics are discussed. As theoretical framework, the scale decomposition of the dynamical equations for neutral fluids by means of spatial filtering is explained. For cosmological applications, the filtered equations in comoving coordinates are also presented. To obtain a closed set of equations that can be evolved in LES, several subgrid scale models for the interactions between numerically resolved and unresolved scales are discussed, in particular the subgrid scale turbulence energy equation model. It is then shown how model coefficients can be calculated, either by dynamical procedures or, a priori, from high-resolution data. For astrophysical applications, adaptive mesh refinement is often indispensable. It is shown that the subgrid scale turbulence energy model allows for a particularly elegant and physically well motivated way of preserving momentum and energy conservation in AMR simulations. Moreover, the notion of shear-improved models for inhomogeneous and non-stationary turbulence is introduced. Finally, applications of LES to turbulent combustion in thermonuclear supernovae, star formation and feedback in galaxies, and cosmological structure formation are reviewed.arXiv:1404.2483v1 [astro-ph.CO] 9 Apr 2014 tial subrange is very narrow for computationally feasible resolutions because the bottleneck effect distorts the spectrum over a large range of high wave numbers below the Nyquist wavenumber [30,27,114]. It appears that LES with an explicit SGS model, such as the K-equation model, can reduce the bottleneck effect to some degree and reproduce scalings from ILES or DNS at lower resolution [45,128,109]. However, more systematic studies covering the parameters space of forced compressible turbulence are necessary to confirm this effect.There are, of course, alternative methods of scale separation and a large variety of SGS models (for a comprehensive overview, see the monographs [103,39]). An example are the Camassa-Holm equations, which follow from the incompressible Navier-Stokes equations by decomposing the trajectories of fluid elements into mean and fluctuating parts in the Lagrangian framework [21]. Since the filtered component of the velocity is defined by an inverse Helmholtz operator of the form (1 − α 2 ∇ 2 ) −1 , which is explicitly applied to determine the turbulent stresses in the filtered velocity equation, the resulting model is called Lagrangian-averaged Navier-Stokes α-model (LANS-α). Depending on the choice of α, the variables computed in LES based on LANS-α are typically smoothed over length scales somewhat larger than the grid resolution. In other words, this type of simulation partially resolves the sub-filter scales, which improves the controllability of the model. While there is no handle on the competition between the SGS model and numerical truncation errors on the grid scale in convectional LES, LANS-α can, in principle, alleviate this problem by adjusting the balance between ...

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Magnetic fields in galaxy clusters

Cited by 10 publications

References 50 publications

Baryonic Processes in the Large-Scale Structuring of the Universe

Baryonic Processes in the Large-Scale Structuring of the Universe

The numerical modelling of MHD astrophysical flows with chemistry

Large Eddy Simulations in Astrophysics

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