Cluster magnetic fields from galactic outflows

By Julius Donnert, Klaus Dolag, H. Lesch, E. R. Müller. 2008

151 citations recorded by the source corpus.

We performed cosmological, magnetohydrodynamical simulations to follow the evolution of magnetic fields in galaxy clusters, exploring the possibility that the origin of the magnetic seed fields is galactic outflows during the starburst phase of galactic evolution. To do this, we coupled a semi-analytical model for magnetized galactic winds as suggested by Bertone, Vogt & Enslin to our cosmological simulation. We find that the strength and structure of magnetic fields observed in galaxy clusters are well reproduced for a wide range of model parameters for the magnetized, galactic winds and do only weakly depend on the exact magnetic structure within the assumed galactic outflows. Although the evolution of a primordial magnetic seed field shows no significant differences to that of galaxy cluster fields from previous studies, we find that the magnetic field pollution in the diffuse medium within filaments is below the level predicted by scenarios with pure primordial magnetic seed field. We therefore conclude that magnetized galactic outflows and their subsequent evolution within the intracluster medium can fully account for the observed magnetic fields in galaxy clusters. Our findings also suggest that measuring cosmological magnetic fields in low-density environments such as filaments is much more useful than observing cluster magnetic fields to infer their possible origin.

Subfields: Astronomy and Astrophysics, Electrical and Electronic Engineering, Instrumentation

View Paper: https://www.semanticscholar.org/paper/fee343516e118df7ecfc8b97aab1c26dcd30b10b

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Citations in the corpus

BLAZARS AS ULTRA-HIGH-ENERGY COSMIC-RAY SOURCES: IMPLICATIONS FOR TeV GAMMA-RAY OBSERVATIONS (2011, background): “…1 µG (e.g., Vallée 2004), and recent simulations have suggested that filaments haveBEG ∼ 1− 10 nG (Ryu et al. 2008; Das et al. 2008, and see also, e.g., Donnert et al. 2009), which are larger than levels expected for the IGMF in voids, and galaxies including AGN are likely located in these…”
LOWER LIMIT ON THE STRENGTH AND FILLING FACTOR OF EXTRAGALACTIC MAGNETIC FIELDS (2011, methodology): “To mimic the even more complex situation in the presence of cosmological structures, we have used magnetic fields derived from several cosmological MHD simulations using constrained initial conditions (Dolag et al. 2005; Donnert et al. 2009; for alternative simulations see, e.g., Ryu et al. 2008).”
The Coma cluster magnetic field from Faraday rotation measures (2009, background): “…from magneto-hydrodynamical simulations performed with different codes (Dolag et al. 1999, 2005; Brueggen et al. 2005, Dubois et al. 2008, Collins et al. 2009, Dolag & Stasyszyn 2008, Donnert et al. 2009a), as a result of the compression of thermal plasma during the cluster gravitational collapse.”
Constraints on the distribution and energetics of fast radio bursts using cosmological hydrodynamic simulations (2014, background): “Such data can provide direct measurements of the magnetisation of the IGM (Cordes et al. 2004), and hence can potentially discriminate between different mechanisms for the origin of cosmic magnetism (e.g., Donnert et al. 2009).”
The Astrophysics of Ultrahigh-Energy Cosmic Rays (2011, methodology): “With these methods, magnetic fields generated by astrophysical feedback can be hard to implement (see, however Donnert et al. 2009 who have incorporated some of these effects).”
Adding helicity to inflationary magnetogenesis (2014, background): “On the other hand, it is not excluded that such fields could be explained simply by ejection of galactic magnetic fields, which are then processed by small scale turbulence in the intra-cluster medium and amplified up to the microGauss level [59].”
Cosmological Magnetic Fields: Their Generation, Evolution and Observation (2013, methodology): “Donnert et al (2009) further developed the model of Bertone et al (2006) and performed simulations aimed at testing the hypothesis of the origin of magnetic fields in galaxy clusters from galactic outflows.”
Massive and refined - II. The statistical properties of turbulent motions in massive galaxy clusters with high spatial resolution (2010, background): “The magnetic ﬁeld is also expected to play a role along the cluster evolution (e.g. Dolag 2006; Dubois & Teyssier 2008;Dolag & Stasyszyn 2009; Donnert et al. 2009; Collins et al. 2010), even if without a ﬀ ecting the spectral properties out-lined in Sec.3.3 for a wide range of scales (e.g. Xu et…”