Turbulent heating in_galaxy_clusters_brightest_in_x_rays

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Turbulent Heating in Galaxy Clusters Brightest in X-rays
I. Zhuravleva1,2, E. Churazov3,4, A. A. Schekochihin5,6, S. W. A...

Perseus and Virgo/M87 are well studied nearby cool-core clusters of galaxies in which
the central cooling times, due to t...

of the second scenario (which may be argued to be more likely if the stirring of the ICM by the
AGN ejecta is of sufficie...

rate: accounting for our convention k=1/l=k1/2π and V1,k=[2k1E(k1)/3]1/2, we obtain Qturb=
ρ0ε=CQ ρ0V1,k
3k, where CQ=33...

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Page 5 of 22
amplitudes.
Modulo this caveat, the approximate balance of cooling and heating (Fig. 3) suggests that
turb...

buoyant bubbles in M87. Astrophys. J., 554, 261-273 (2001).
11. Omma, H., Binney, J., Bryan, G. & Slyz, A. Heating coolin...

24. Schekochihin, A. A. et al. Astrophysical gyrokinetics: kinetic and fluid turbulent cascades in
magnetized weakly coll...

Figure 1 | X-ray image of the core of the Perseus Cluster. (a) X-ray surface brightness in units
of counts/s/pixel obtain...

Figure 2 | Measured amplitude of the one-component velocity V1,k of gas motions versus
wavenumber k. The amplitude is sho...

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Figure 3 | Turbulent heating (Qheat) versus gas cooling (Qcool) rates in the Perseus and Virgo
cores. Each shaded rectang...

The X-ray mosaic image and its reduced counterpart for the Virgo Cluster are shown in
Extended Data Fig. 2. The 0.5-3.5 k...

The cooling time tcool and the cooling rate Qcool have been calculated using a gas cooling
function Λn(T) with solar meta...

As the density explicitly enters the expressions for both the cooling rate and turbulent heating
rate, the linear correla...

including the case of the simplest β model. This is why we expect that the estimates of the
heating power based on small-...

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weights have larger statistical errors, but provide a more uniform scheme for evaluating the
amplitudes of the surface br...

large scales at all scales l<lO, where the density becomes a passive scalar13.
Assuming that radiative cooling is balance...

surface brightness15. The observed morphology of these features, namely narrow in the radial
direction and wide in the az...

31. Churazov, E., Forman, W., Jones, C. & Böhringer, H. XMM-Newton observations of the
Perseus Cluster. I. The temperatur...

45. Lufkin, E. A., Balbus, S. A. & Hawley, J. F. Nonlinear evolution of internal gravity waves in
cluster cooling flows. ...

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Extended Data Figure 1 | Thermodynamic properties of the Perseus and Virgo Clusters.
Radial profiles of the deprojected e...

Extended Data Figure 2 | X-ray image of the core of the Virgo Cluster. (a) X-ray surface
brightness in units of counts/s/...

Extended Data Figure 4 | Turbulent heating per unit density versus radiative cooling per
unit density and the Ozmidov sca...

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